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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Roman-Lopes%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Roman-Lopes%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Roman-Lopes%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Roman-Lopes%2C+A&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.16646">arXiv:2406.16646</a> <span> [<a href="https://arxiv.org/pdf/2406.16646">pdf</a>, <a href="https://arxiv.org/format/2406.16646">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450584">10.1051/0004-6361/202450584 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VISTA Variables in the V铆a L谩ctea eXtended (VVVX) ESO public survey: Completion of the observations and legacy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garc%C3%ADa%2C+J">J. Alonso-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+S">S. Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=Baravalle%2C+L">L. Baravalle</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Caceres%2C+C">C. Caceres</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%C3%A9%2C+A+N">A. N. Chen茅</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Duplancic%2C+F">F. Duplancic</a>, <a href="/search/astro-ph?searchtype=author&query=Garro%2C+E+R">E. R. Garro</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez%2C+M">M. G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Luna%2C+A">A. Luna</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">D. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+M+G">M. G. Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Pullen%2C+J+B">J. B. Pullen</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+J+L">J. L. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+L+C">L. C. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Albino%2C+P+H+C">P. H. C. Albino</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+M+V">M. V. Alonso</a> , et al. (121 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.16646v1-abstract-short" style="display: inline;"> The ESO public survey VISTA Variables in the V铆a L谩ctea (VVV) surveyed the inner Galactic bulge and the adjacent southern Galactic disk from $2009-2015$. Upon its conclusion, the complementary VVV eXtended (VVVX) survey has expanded both the temporal as well as spatial coverage of the original VVV area, widening it from $562$ to $1700$ sq. deg., as well as providing additional epochs in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.16646v1-abstract-full').style.display = 'inline'; document.getElementById('2406.16646v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.16646v1-abstract-full" style="display: none;"> The ESO public survey VISTA Variables in the V铆a L谩ctea (VVV) surveyed the inner Galactic bulge and the adjacent southern Galactic disk from $2009-2015$. Upon its conclusion, the complementary VVV eXtended (VVVX) survey has expanded both the temporal as well as spatial coverage of the original VVV area, widening it from $562$ to $1700$ sq. deg., as well as providing additional epochs in $JHK_{\rm s}$ filters from $2016-2023$. With the completion of VVVX observations during the first semester of 2023, we present here the observing strategy, a description of data quality and access, and the legacy of VVVX. VVVX took $\sim 2000$ hours, covering about 4% of the sky in the bulge and southern disk. VVVX covered most of the gaps left between the VVV and the VISTA Hemisphere Survey (VHS) areas and extended the VVV time baseline in the obscured regions affected by high extinction and hence hidden from optical observations. VVVX provides a deep $JHK_{\rm s}$ catalogue of $\gtrsim 1.5\times10^9$ point sources, as well as a $K_{\rm s}$ band catalogue of $\sim 10^7$ variable sources. Within the existing VVV area, we produced a $5D$ map of the surveyed region by combining positions, distances, and proper motions of well-understood distance indicators such as red clump stars, RR Lyrae, and Cepheid variables. In March 2023 we successfully finished the VVVX survey observations that started in 2016, an accomplishment for ESO Paranal Observatory upon 4200 hours of observations for VVV+VVVX. The VVV+VVVX catalogues complement those from the Gaia mission at low Galactic latitudes and provide spectroscopic targets for the forthcoming ESO high-multiplex spectrographs MOONS and 4MOST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.16646v1-abstract-full').style.display = 'none'; document.getElementById('2406.16646v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 11 figures (+ appendix). Accepted for publication in Astronomy and Astrophysics in section 14: Catalogs and data</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A148 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.16178">arXiv:2404.16178</a> <span> [<a href="https://arxiv.org/pdf/2404.16178">pdf</a>, <a href="https://arxiv.org/format/2404.16178">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Unveiling very young O stars. Two Galactic O2V((f*))z in Westerlund 2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">A. Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.16178v1-abstract-short" style="display: inline;"> O-type stars are known to significantly contribute to both the dynamics and evolution of galaxies. Massive and luminous, they probably control and regulate the galaxies star formation rates. For this work I performed a redetermination of the spectral types and effective temperatures of the Galactic O-type stars MSP182, MSP183, MSP199, VPHAS-01338, and VPHAS-01273. From a careful examination of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.16178v1-abstract-full').style.display = 'inline'; document.getElementById('2404.16178v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.16178v1-abstract-full" style="display: none;"> O-type stars are known to significantly contribute to both the dynamics and evolution of galaxies. Massive and luminous, they probably control and regulate the galaxies star formation rates. For this work I performed a redetermination of the spectral types and effective temperatures of the Galactic O-type stars MSP182, MSP183, MSP199, VPHAS-01338, and VPHAS-01273. From a careful examination of the spectral features present in the blue optical spectral region, it was possible to identify several nitrogen lines usually only seen in the blue optical spectra of O2-O3 stars. From the nitrogen ionic equivalent width ratios measured in the spectra of MSP182, MSP183, MSP199, VPHAS-01338, and VPHAS-01273, and in those of standard stars of the O2-O4 spectral types, earlier spectral types and hotter effective temperature values were derived. Two O2V, together with three new O3V stars, are now firmly identified in the Westerlund 2 region. Besides RFS1 in NGC3603, the O2 stars found in Westerlund 2 are the only other exemplars known to date in the Milky Way. From the nitrogen equivalent width line ratios measured in the spectra of standard stars of the O2-O4 spectral types, linear relations between the NIV4058-NIII4640 ratio and the effective temperature in the 47000K-51000K range were derived. Based on my spectroscopic analysis of the science targets and the use of a HRD, a mean heliocentric distance of 5kpc to Westerlund 2 was computed, a result that is in line with the mean heliocentric distance of 5.3(1.5) kpc obtained from the associated Gaia DR3 parallaxes and distances. The Westerlund 2 massive stars studied in this work probably share a common evolutionary process that might be representative of the evolutionary ages of a large fraction of the cluster's O-type stellar population, which seems to be much younger than 1 Myrs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.16178v1-abstract-full').style.display = 'none'; document.getElementById('2404.16178v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 5 figures, accepted for publication in Astronomy and Astrophysics (DOI(pending):10.1051/0004-6361/202449474)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.07505">arXiv:2403.07505</a> <span> [<a href="https://arxiv.org/pdf/2403.07505">pdf</a>, <a href="https://arxiv.org/format/2403.07505">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Rotational Evolution of Classical T Tauri Stars: Models and Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Serna%2C+J">Javier Serna</a>, <a href="/search/astro-ph?searchtype=author&query=Pinz%C3%B3n%2C+G">Giovanni Pinz贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">Jes煤s Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Manzo-Mart%C3%ADnez%2C+E">Ezequiel Manzo-Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Mauco%2C+K">Karina Mauco</a>, <a href="/search/astro-ph?searchtype=author&query=Rom%C3%A1n-Z%C3%BA%C3%B1iga%2C+C+G">Carlos G. Rom谩n-Z煤帽iga</a>, <a href="/search/astro-ph?searchtype=author&query=Calvet%2C+N">Nuria Calvet</a>, <a href="/search/astro-ph?searchtype=author&query=Brice%C3%B1o%2C+C">Cesar Brice帽o</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Valdivia%2C+R">Ricardo L贸pez-Valdivia</a>, <a href="/search/astro-ph?searchtype=author&query=Kounkel%2C+M">Marina Kounkel</a>, <a href="/search/astro-ph?searchtype=author&query=Stringfellow%2C+G+S">Guy S. Stringfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Pinsonneault%2C+M">Marc Pinsonneault</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+L">Lucia Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+L">Lyra Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Covey%2C+K">Kevin Covey</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">Amelia Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.07505v1-abstract-short" style="display: inline;"> We developed a grid of stellar rotation models for low-mass and solar-type Classical T Tauri stars (CTTS) ($0.3M_{\odot}<M_{\ast}<1.2M_{\odot}$). These models incorporate the star-disk interaction and magnetospheric ejections to investigate the evolution of the stellar rotation rate as a function of the mass of the star $M_{\ast}$, the magnetic field ($B_{\ast}$), and stellar wind (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.07505v1-abstract-full').style.display = 'inline'; document.getElementById('2403.07505v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.07505v1-abstract-full" style="display: none;"> We developed a grid of stellar rotation models for low-mass and solar-type Classical T Tauri stars (CTTS) ($0.3M_{\odot}<M_{\ast}<1.2M_{\odot}$). These models incorporate the star-disk interaction and magnetospheric ejections to investigate the evolution of the stellar rotation rate as a function of the mass of the star $M_{\ast}$, the magnetic field ($B_{\ast}$), and stellar wind ($\dot{M}_{wind}$). We compiled and determined stellar parameters for 208 CTTS, such as projected rotational velocity $v\sin(i)$, mass accretion rate $\dot{M}_{acc}$, stellar mass $M_{\ast}$, ages, and estimated rotational periods using TESS data. We also estimated a representative value of the mass-loss rate for our sample using the $[\text{O}\text{ I}]$ spectral line. Our results confirm that $v\sin(i)$ measurements in CTTS agree with the rotation rates provided by our spin models in the accretion-powered stellar winds (APSW) picture. In addition, we used the Approximate Bayesian Computation (ABC) technique to explore the connection between the model parameters and the observational properties of CTTS. We find that the evolution of $v\sin(i)$ with age might be regulated by variations in (1) the intensity of $B_{\ast}$ and (2) the fraction of the accretion flow ejected in magnetic winds, removing angular momentum from these systems. The youngest stars in our sample ($\sim $1 Myr) show a median branching ratio $\dot{M}_{wind}/\dot{M}_{acc}\sim$ $0.16$ and median $B_{\ast}\sim$ 2000 G, in contrast to $\sim 0.01$ and 1000 G, respectively, for stars with ages $\gtrsim 3$ Myr. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.07505v1-abstract-full').style.display = 'none'; document.getElementById('2403.07505v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 18 figures, Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.08970">arXiv:2311.08970</a> <span> [<a href="https://arxiv.org/pdf/2311.08970">pdf</a>, <a href="https://arxiv.org/format/2311.08970">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Physics and Society">physics.soc-ph</span> </div> </div> <p class="title is-5 mathjax"> SDSS-IV from 2014 to 2016: A Detailed Demographic Comparison over Three Years </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jones%2C+A+M">Amy M. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Cherinka%2C+B+A">Brian A. Cherinka</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">Karen L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Lucatello%2C+S">Sara Lucatello</a>, <a href="/search/astro-ph?searchtype=author&query=Diamond-Stanic%2C+A+M">Aleksandar M. Diamond-Stanic</a>, <a href="/search/astro-ph?searchtype=author&query=Bird%2C+S+A">Sarah A. Bird</a>, <a href="/search/astro-ph?searchtype=author&query=Blanton%2C+M+R">Michael R. Blanton</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Farr%2C+E+E">Emily E. Farr</a>, <a href="/search/astro-ph?searchtype=author&query=Feuillet%2C+D">Diane Feuillet</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P+M">Peter M. Frinchaboy</a>, <a href="/search/astro-ph?searchtype=author&query=Hagen%2C+A">Alex Hagen</a>, <a href="/search/astro-ph?searchtype=author&query=Kinemuchi%2C+K">Karen Kinemuchi</a>, <a href="/search/astro-ph?searchtype=author&query=Lundgren%2C+B">Britt Lundgren</a>, <a href="/search/astro-ph?searchtype=author&query=Marinelli%2C+M+L">Mariarosa L. Marinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Myers%2C+A+D">Adam D. Myers</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">Ashley J. Ross</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Gallego%2C+J+R">Jose R. Sanchez-Gallego</a>, <a href="/search/astro-ph?searchtype=author&query=Schmidt%2C+S+J">Sarah J. Schmidt</a>, <a href="/search/astro-ph?searchtype=author&query=Sobeck%2C+J">Jennifer Sobeck</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Tayar%2C+J">Jamie Tayar</a>, <a href="/search/astro-ph?searchtype=author&query=Vargas-Magana%2C+M">Mariana Vargas-Magana</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.08970v1-abstract-short" style="display: inline;"> The Sloan Digital Sky Survey (SDSS) is one of the largest international astronomy organizations. We present demographic data based on surveys of its members from 2014, 2015 and 2016, during the fourth phase of SDSS (SDSS-IV). We find about half of SDSS-IV collaboration members were based in North America, a quarter in Europe, and the remainder in Asia and Central and South America. Overall, 26-36%… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.08970v1-abstract-full').style.display = 'inline'; document.getElementById('2311.08970v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.08970v1-abstract-full" style="display: none;"> The Sloan Digital Sky Survey (SDSS) is one of the largest international astronomy organizations. We present demographic data based on surveys of its members from 2014, 2015 and 2016, during the fourth phase of SDSS (SDSS-IV). We find about half of SDSS-IV collaboration members were based in North America, a quarter in Europe, and the remainder in Asia and Central and South America. Overall, 26-36% are women (from 2014 to 2016), up to 2% report non-binary genders. 11-14% report that they are racial or ethnic minorities where they live. The fraction of women drops with seniority, and is also lower among collaboration leadership. Men in SDSS-IV were more likely to report being in a leadership role, and for the role to be funded and formally recognized. SDSS-IV collaboration members are twice as likely to have a parent with a college degree, than the general population, and are ten times more likely to have a parent with a PhD. This trend is slightly enhanced for female collaboration members. Despite this, the fraction of first generation college students (FGCS) is significant (31%). This fraction increased among collaboration members who are racial or ethnic minorities (40-50%), and decreased among women (15-25%). SDSS-IV implemented many inclusive policies and established a dedicated committee, the Committee on INclusiveness in SDSS (COINS). More than 60% of the collaboration agree that the collaboration is inclusive; however, collaboration leadership more strongly agree with this than the general membership. In this paper, we explain these results in full, including the history of inclusive efforts in SDSS-IV. We conclude with a list of suggested recommendations based on our findings, which can be used to improve equity and inclusion in large astronomical collaborations, which we argue is not only moral, but will also optimize their scientific output. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.08970v1-abstract-full').style.display = 'none'; document.getElementById('2311.08970v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 9 figures, accepted in PASP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.12503">arXiv:2309.12503</a> <span> [<a href="https://arxiv.org/pdf/2309.12503">pdf</a>, <a href="https://arxiv.org/format/2309.12503">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Revealing the Chemical Structure of the Magellanic Clouds with APOGEE. II. Abundance Gradients of the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Povick%2C+J+T">Joshua T. Povick</a>, <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D+L">David L. Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Cioni%2C+M+L">Maria-Rosa L. Cioni</a>, <a href="/search/astro-ph?searchtype=author&query=Yuxi"> Yuxi</a>, <a href="/search/astro-ph?searchtype=author&query=Lu"> Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+R">Ricardo Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Stringfellow%2C+G+S">Guy S. Stringfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+A">Andr茅s Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Longa-Pe%C3%B1a%2C+P">Pen茅lope Longa-Pe帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.12503v1-abstract-short" style="display: inline;"> We present the abundance gradients of the Large Magellanic Cloud (LMC) for 25 elemental abundance ratios and their respective temporal evolution as well as age-[X/Fe] trends using 6130 LMC field red giant branch (RGB) stars observed by SDSS-IV / APOGEE-2S. APOGEE is a high resolution ($R$ $\sim$22,500) $H$-band spectroscopic survey that gathered data on the LMC with broad radial and azimuthal cove… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12503v1-abstract-full').style.display = 'inline'; document.getElementById('2309.12503v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.12503v1-abstract-full" style="display: none;"> We present the abundance gradients of the Large Magellanic Cloud (LMC) for 25 elemental abundance ratios and their respective temporal evolution as well as age-[X/Fe] trends using 6130 LMC field red giant branch (RGB) stars observed by SDSS-IV / APOGEE-2S. APOGEE is a high resolution ($R$ $\sim$22,500) $H$-band spectroscopic survey that gathered data on the LMC with broad radial and azimuthal coverage out to $\sim$10\degr. The calculated overall metallicity gradient of the LMC with no age binning is $-$0.0380 $\pm$ 0.0022 dex/kpc. We also find that many of the abundance gradients show a U-shaped trend as functions of age. This trend is marked by a flattening of the gradient but then a general steepening at more recent times. The extreme point at which all these gradients (with the U-shaped trend) begin to steepen is $\gtrsim$2 Gyr ago. In addition, some of the age-[X/Fe] trends show an increase starting a few Gyr before the extreme point in the gradient evolutions. A subset of the age-[X/Fe] trends also show maxima concurrent with the gradients' extreme points, further pinpointing a major event in the history of the LMC $\sim$2 Gyr ago. This time frame is consistent with a previously proposed interaction between the Magellanic Clouds suggesting that this is most likely the cause of the distinct trend in the gradients and age-[X/Fe] trends. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12503v1-abstract-full').style.display = 'none'; document.getElementById('2309.12503v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 19 figures, and 10 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.17333">arXiv:2306.17333</a> <span> [<a href="https://arxiv.org/pdf/2306.17333">pdf</a>, <a href="https://arxiv.org/format/2306.17333">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1538-3873/ace3f7">10.1088/1538-3873/ace3f7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Rubin Observatory LSST Stars Milky Way and Local Volume Star Clusters Roadmap </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Usher%2C+C">Christopher Usher</a>, <a href="/search/astro-ph?searchtype=author&query=Dage%2C+K+C">Kristen C. Dage</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+L">L茅o Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Barmby%2C+P">Pauline Barmby</a>, <a href="/search/astro-ph?searchtype=author&query=Bonatto%2C+C+J">Charles J. Bonatto</a>, <a href="/search/astro-ph?searchtype=author&query=Chies-Santos%2C+A+L">Ana L. Chies-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Clarkson%2C+W+I">William I. Clarkson</a>, <a href="/search/astro-ph?searchtype=author&query=Camus%2C+M+G">Matias G贸mez Camus</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+E+A">Eduardo A. Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A+M+N">Annette M. N. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Pieres%2C+A">Adriano Pieres</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">Loredana Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Rhode%2C+K+L">Katherine L. Rhode</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+R+M">R. Michael Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">Vincenzo Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Santiago%2C+B">Basilio Santiago</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Street%2C+R+A">R. A. Street</a>, <a href="/search/astro-ph?searchtype=author&query=Szab%C3%B3%2C+R">R贸bert Szab贸</a>, <a href="/search/astro-ph?searchtype=author&query=Venuti%2C+L">Laura Venuti</a>, <a href="/search/astro-ph?searchtype=author&query=Zaggia%2C+S">Simone Zaggia</a>, <a href="/search/astro-ph?searchtype=author&query=Canossa%2C+M">Marco Canossa</a>, <a href="/search/astro-ph?searchtype=author&query=Floriano%2C+P">Pedro Floriano</a>, <a href="/search/astro-ph?searchtype=author&query=Lopes%2C+P">Pedro Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Miranda%2C+N+L">Nicole L. Miranda</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.17333v1-abstract-short" style="display: inline;"> The Vera C. Rubin Observatory will undertake the Legacy Survey of Space and Time, providing an unprecedented, volume-limited catalog of star clusters in the Southern Sky, including Galactic and extragalactic star clusters. The Star Clusters subgroup of the Stars, Milky Way and Local Volume Working Group has identified key areas where Rubin Observatory will enable significant progress in star clust… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17333v1-abstract-full').style.display = 'inline'; document.getElementById('2306.17333v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.17333v1-abstract-full" style="display: none;"> The Vera C. Rubin Observatory will undertake the Legacy Survey of Space and Time, providing an unprecedented, volume-limited catalog of star clusters in the Southern Sky, including Galactic and extragalactic star clusters. The Star Clusters subgroup of the Stars, Milky Way and Local Volume Working Group has identified key areas where Rubin Observatory will enable significant progress in star cluster research. This roadmap represents our science cases and preparation for studies of all kinds of star clusters from the Milky Way out to distances of tens of megaparsecs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17333v1-abstract-full').style.display = 'none'; document.getElementById('2306.17333v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted to PASP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.06348">arXiv:2306.06348</a> <span> [<a href="https://arxiv.org/pdf/2306.06348">pdf</a>, <a href="https://arxiv.org/format/2306.06348">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Revealing the Chemical Structure of the Magellanic Clouds with APOGEE. I. Calculating Individual Stellar Ages of RGB Stars in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Povick%2C+J+T">Joshua T. Povick</a>, <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D+L">David L. Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Massana%2C+P">Pol Massana</a>, <a href="/search/astro-ph?searchtype=author&query=Tayar%2C+J">Jamie Tayar</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K+A+G">Knut A. G. Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Cioni%2C+M+L">Maria-Rosa L. Cioni</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Carrera%2C+R">Ricardo Carrera</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+Y">Yumi Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+A">Andr茅s Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+V+V">Verne V. Smith</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.06348v1-abstract-short" style="display: inline;"> Stellar ages are critical for understanding the temporal evolution of a galaxy. We calculate the ages of over 6000 red giant branch stars in the Large Magellanic Cloud (LMC) observed with SDSS-IV / APOGEE-S. Ages are derived using multi-band photometry, spectroscopic parameters (T$_\text{eff}$, $\log{g}$, [Fe/H], and [$伪$/Fe]) and stellar isochrones and the assumption that the stars lie in a thin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06348v1-abstract-full').style.display = 'inline'; document.getElementById('2306.06348v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06348v1-abstract-full" style="display: none;"> Stellar ages are critical for understanding the temporal evolution of a galaxy. We calculate the ages of over 6000 red giant branch stars in the Large Magellanic Cloud (LMC) observed with SDSS-IV / APOGEE-S. Ages are derived using multi-band photometry, spectroscopic parameters (T$_\text{eff}$, $\log{g}$, [Fe/H], and [$伪$/Fe]) and stellar isochrones and the assumption that the stars lie in a thin inclined plane to get accurate distances. The isochrone age and extinction are varied until a best match is found for the observed photometry. We perform validation using the APOKASC sample, which has asteroseismic masses and accurate ages, and find that our uncertainties are $\sim$20% and range from $\sim$1$-$3 Gyr for the calculated age values. Here we present the LMC age map as well as the age-radius relation and an accurate age-metallicity relation (AMR). The age map and age-radius relation reveal that recent star formation in the galaxy was more centrally located and that there is a slight dichotomy between the north and south with the northern fields being slightly younger. The northern fields that cover a known spiral arm have median ages of $\gtrsim$ 2 Gyr, which is the time when an interaction with the SMC is suggested to have happened. The AMR is mostly flat especially for older ages although recently (about 2.0-2.5 Gyr ago) there is an increase in the median [Fe/H]. Based on the time frame, this might also be attributed to the close interaction between the LMC and SMC. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06348v1-abstract-full').style.display = 'none'; document.getElementById('2306.06348v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 22 figures, submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.19460">arXiv:2305.19460</a> <span> [<a href="https://arxiv.org/pdf/2305.19460">pdf</a>, <a href="https://arxiv.org/format/2305.19460">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347046">10.1051/0004-6361/202347046 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chemo-Dynamical Tagging in the Outskirts: The Origins of Stellar Substructures in the Magellanic Clouds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+C">C茅sar Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Monachesi%2C+A">Antonela Monachesi</a>, <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D+L">David L. Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+X">Xinlun Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">Knut Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+Y">Yumi Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Zivick%2C+P">Paul Zivick</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Douglas Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+A">Andres Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+R+R">Ricardo R. Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.19460v2-abstract-short" style="display: inline;"> We present the first detailed chemical analysis from APOGEE-2S observations of stars in six regions of recently discovered substructures in the outskirts of the Magellanic Clouds extending to 20 degrees from the LMC center. We also present, for the first time, the metallicity and alpha-abundance radial gradients of the LMC and SMC out to 11 degrees and 6 degrees, respectively. Our chemical tagging… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.19460v2-abstract-full').style.display = 'inline'; document.getElementById('2305.19460v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.19460v2-abstract-full" style="display: none;"> We present the first detailed chemical analysis from APOGEE-2S observations of stars in six regions of recently discovered substructures in the outskirts of the Magellanic Clouds extending to 20 degrees from the LMC center. We also present, for the first time, the metallicity and alpha-abundance radial gradients of the LMC and SMC out to 11 degrees and 6 degrees, respectively. Our chemical tagging includes 13 species including light, alpha, and Fe-peak elements. We find that the abundances of all of these chemical elements in stars populating two regions in the northern periphery - along the northern "stream"-like feature - show good agreement with the chemical patterns of the LMC, and thus likely have an LMC origin. For substructures located in the southern periphery of the LMC, we find more complex chemical and kinematical signatures, indicative of a mix of LMC-like and SMC-like populations. However, the southern region closest to the LMC shows better agreement with the LMC, whereas that closest to the SMC shows a much better agreement with the SMC chemical pattern. When combining this information with 3-D kinematical information for these stars, we conclude that the southern region closest to the LMC has likely an LMC origin, whereas that closest to the SMC has an SMC origin, and the other two southern regions have a mix of LMC and SMC origins. Our results add to the evidence that the southern substructures of the LMC periphery are the product of close interactions between the LMC and SMC, and thus likely hold important clues that can constrain models of their detailed dynamical histories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.19460v2-abstract-full').style.display = 'none'; document.getElementById('2305.19460v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 15 figures, 9 tables; Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 680, A79 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.13371">arXiv:2305.13371</a> <span> [<a href="https://arxiv.org/pdf/2305.13371">pdf</a>, <a href="https://arxiv.org/format/2305.13371">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Cataclysmic Variables from Sloan Digital Sky Survey V -- the search for period bouncers continues </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Inight%2C+K">K. Inight</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A4nsicke%2C+B+T">Boris T. G盲nsicke</a>, <a href="/search/astro-ph?searchtype=author&query=Schwope%2C+A">A. Schwope</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S+F">S. F. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Badenes%2C+C">C. Badenes</a>, <a href="/search/astro-ph?searchtype=author&query=Breedt%2C+E">E. Breedt</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+V">V. Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+B+D+R">B. D. R. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Fusillo%2C+N+P+G">N. P. Gentile Fusillo</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+M+J">M. J. Green</a>, <a href="/search/astro-ph?searchtype=author&query=Hermes%2C+J+J">J. J. Hermes</a>, <a href="/search/astro-ph?searchtype=author&query=Huamani%2C+I+A">I. Achaica Huamani</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+H">H. Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Knauff%2C+K">K. Knauff</a>, <a href="/search/astro-ph?searchtype=author&query=Kurpas%2C+J">J. Kurpas</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+K+S">K. S. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Malanushenko%2C+V">V. Malanushenko</a>, <a href="/search/astro-ph?searchtype=author&query=Morrison%2C+S">S. Morrison</a>, <a href="/search/astro-ph?searchtype=author&query=C.%2C+I+J+Q">I. J. Quiroz C.</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+G+N+A">G. N. Aichele Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">A. Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Schreiber%2C+M+R">M. R. Schreiber</a>, <a href="/search/astro-ph?searchtype=author&query=Standke%2C+A">A. Standke</a>, <a href="/search/astro-ph?searchtype=author&query=St%C3%BCtz%2C+L">L. St眉tz</a>, <a href="/search/astro-ph?searchtype=author&query=Thorstensen%2C+J+R">J. R. Thorstensen</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.13371v2-abstract-short" style="display: inline;"> SDSS-V is carrying out a dedicated survey for white dwarfs, single and in binaries, and we report the analysis of the spectroscopy of cataclysmic variables (CVs) and CV candidates obtained during the final plug plate observations of SDSS. We identify eight new CVs, spectroscopically confirm 53 and refute eleven published CV candidates, and we report 21 new or improved orbital periods. Combined wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.13371v2-abstract-full').style.display = 'inline'; document.getElementById('2305.13371v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.13371v2-abstract-full" style="display: none;"> SDSS-V is carrying out a dedicated survey for white dwarfs, single and in binaries, and we report the analysis of the spectroscopy of cataclysmic variables (CVs) and CV candidates obtained during the final plug plate observations of SDSS. We identify eight new CVs, spectroscopically confirm 53 and refute eleven published CV candidates, and we report 21 new or improved orbital periods. Combined with previously published data, the orbital period distribution of the SDSS-V CVs does not clearly exhibit a period gap. This is consistent with previous findings that spectroscopically identified CVs have a larger proportion of short-period systems compared to samples identified from photometric variability. Remarkably, despite a systematic search, we find very few period bouncers. We estimate the space density of period bouncers to be $\simeq0.2\times10^{-6}\,\mathrm{pc}^{-3}$, i.e. they represent only a few per cent of the total CV population. This suggests that during their final phase of evolution, CVs either destroy the donor, e.g. via a merger, or that they become detached and cease mass transfer. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.13371v2-abstract-full').style.display = 'none'; document.getElementById('2305.13371v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by MNRAS. Includes machine readable list of CVs</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2023MNRAS.525.3597I </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.11612">arXiv:2305.11612</a> <span> [<a href="https://arxiv.org/pdf/2305.11612">pdf</a>, <a href="https://arxiv.org/format/2305.11612">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202345856">10.1051/0004-6361/202345856 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sapaki: Galactic O3If* star possibly born in isolation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Plaza%2C+M+S+Z">M. S. Zarricueta Plaza</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">A. Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Sanmartim%2C+D">D. Sanmartim</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.11612v1-abstract-short" style="display: inline;"> Context: The study of high-mass stars found to be isolated in the field of the Milky Way may help to probe the feasibility of the core-accretion mechanism in the case of massive star formation. The existence of truly isolated stars may efficiently probe the possibility that individual massive stars can be born in isolation. Aims: We observed WR67a (hereafter Sapaki), an O3If* star that appears to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.11612v1-abstract-full').style.display = 'inline'; document.getElementById('2305.11612v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.11612v1-abstract-full" style="display: none;"> Context: The study of high-mass stars found to be isolated in the field of the Milky Way may help to probe the feasibility of the core-accretion mechanism in the case of massive star formation. The existence of truly isolated stars may efficiently probe the possibility that individual massive stars can be born in isolation. Aims: We observed WR67a (hereafter Sapaki), an O3If* star that appears to be isolated close to the center of a well-developed giant cavity that is aptly traced by 8.0 $渭$m hot dust emission. Methods: We acquired medium-resolution ($R=4100$) and moderate signal-to-noise ($S/N = 95$ at 4500 脜) spectra for Sapaki in the range of 3800-10500 脜 with the Magellan Echellette (MagE) at Las Campanas Observatory. We computed the line-of-sight total extinctions. Additionally, we restricted its heliocentric distance by using a range of different estimators. Moreover, we measured its radial velocity from several lines in its spectrum. Finally, we analyzed its proper motions from Gaia to examine its possible runaway status. Results: The star has been classified as having the spectral type O3If* given its resemblance to standard examples of the class. In addition, we found that Sapaki is highly obscured, reaching a line-of-sight extinction value of $A_{V} = 7.87$. We estimated the heliocentric distance to be in the range of $d = 4-7$ kpc. We also estimated its radial velocity to be $V_{r} = -34.2 \pm 15.6$ km/s. We may also discard its runaway status solely based on its 2D kinematics. Furthermore, by analyzing proper motions and parallaxes provided by Gaia, we found only one other star with compatible measurements. Conclusions: Given its apparent non-runaway status and the absence of clustering, Sapaki appears to be a solid candidate for isolated high-mass star formation in the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.11612v1-abstract-full').style.display = 'none'; document.getElementById('2305.11612v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 675, A22 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.07186">arXiv:2301.07186</a> <span> [<a href="https://arxiv.org/pdf/2301.07186">pdf</a>, <a href="https://arxiv.org/format/2301.07186">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/acc106">10.3847/1538-4365/acc106 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ABYSS I: Targeting strategy for APOGEE & BOSS young star survey in SDSS-V </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kounkel%2C+M">Marina Kounkel</a>, <a href="/search/astro-ph?searchtype=author&query=Zari%2C+E">Eleonora Zari</a>, <a href="/search/astro-ph?searchtype=author&query=Covey%2C+K">Kevin Covey</a>, <a href="/search/astro-ph?searchtype=author&query=Tkachenko%2C+A">Andrew Tkachenko</a>, <a href="/search/astro-ph?searchtype=author&query=Z%C3%BA%C3%B1iga%2C+C+R">Carlos Rom谩n Z煤帽iga</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K">Keivan Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Stutz%2C+A+M">Amelia M. Stutz</a>, <a href="/search/astro-ph?searchtype=author&query=Stringfellow%2C+G">Guy Stringfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">Jes煤s Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez%2C+K+P">Karla Pe帽a Ram铆rez</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">Amelia Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J+S">Jinyoung Serena Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+L">Lyra Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Kollmeier%2C+J">Juna Kollmeier</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Valdivia%2C+R">Ricardo L贸pez-Valdivia</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Ayala%2C+B">B谩rbara Rojas-Ayala</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.07186v2-abstract-short" style="display: inline;"> The fifth iteration of the Sloan Digital Sky Survey (SDSS-V) is set to obtain optical and near-infrared spectra of $\sim$5 million stars of all ages and masses throughout the Milky Way. As a part of these efforts, APOGEE & BOSS Young Star Survey (ABYSS) will observe $\sim10^5$ stars with ages $<$30 Myr that have been selected using a set of homogeneous selection functions that make use of differen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07186v2-abstract-full').style.display = 'inline'; document.getElementById('2301.07186v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.07186v2-abstract-full" style="display: none;"> The fifth iteration of the Sloan Digital Sky Survey (SDSS-V) is set to obtain optical and near-infrared spectra of $\sim$5 million stars of all ages and masses throughout the Milky Way. As a part of these efforts, APOGEE & BOSS Young Star Survey (ABYSS) will observe $\sim10^5$ stars with ages $<$30 Myr that have been selected using a set of homogeneous selection functions that make use of different tracers of youth. The ABYSS targeting strategy we describe in this paper is aimed to provide the largest spectroscopic census of young stars to-date. It consists of 8 different types of selection criteria that take the position on the HR diagram, infrared excess, variability, as well as the position in phase space in consideration. The resulting catalog of $\sim$200,000 sources (of which a half are expected to be observed) provides representative coverage of the young Galaxy, including both nearby diffuse associations as well as more distant massive complexes, reaching towards the inner Galaxy and the Galactic center. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07186v2-abstract-full').style.display = 'none'; document.getElementById('2301.07186v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 12 pages. Accepted to ApJS. Part of SDSS DR18</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.06454">arXiv:2211.06454</a> <span> [<a href="https://arxiv.org/pdf/2211.06454">pdf</a>, <a href="https://arxiv.org/format/2211.06454">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aca324">10.3847/1538-4357/aca324 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pre-main Sequence Brackett Emitters in the APOGEE DR17 Catalog: Line Strengths and Physical Properties of Accretion Columns </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Campbell%2C+H">Hunter Campbell</a>, <a href="/search/astro-ph?searchtype=author&query=Khilfeh%2C+E">Elliott Khilfeh</a>, <a href="/search/astro-ph?searchtype=author&query=Covey%2C+K+R">Kevin R. Covey</a>, <a href="/search/astro-ph?searchtype=author&query=Kounkel%2C+M">Marina Kounkel</a>, <a href="/search/astro-ph?searchtype=author&query=Ballantyne%2C+R">Richard Ballantyne</a>, <a href="/search/astro-ph?searchtype=author&query=Corey%2C+S">Sabrina Corey</a>, <a href="/search/astro-ph?searchtype=author&query=Rom%C3%A1n-Z%C3%BA%C3%B1iga%2C+C+G">Carlos G. Rom谩n-Z煤帽iga</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">Jes煤s Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez%2C+E+M">Ezequiel Manzo Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez%2C+K+P">Karla Pe帽a Ram铆rez</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Stringfellow%2C+G+S">Guy S. Stringfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">Jura Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Chojnowski%2C+S+D">S. Drew Chojnowski</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez-Preciado%2C+V">Valeria Ram铆rez-Preciado</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J+S">Jinyoung Serena Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Serna%2C+J">Javier Serna</a>, <a href="/search/astro-ph?searchtype=author&query=Stutz%2C+A+M">Amelia M. Stutz</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Valdivia%2C+R">Ricardo L贸pez-Valdivia</a>, <a href="/search/astro-ph?searchtype=author&query=Su%C3%A1rez%2C+G">Genaro Su谩rez</a>, <a href="/search/astro-ph?searchtype=author&query=Ybarra%2C+J+E">Jason E. Ybarra</a>, <a href="/search/astro-ph?searchtype=author&query=Longa-Pe%C3%B1a%2C+P">Pen茅lope Longa-Pe帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.06454v2-abstract-short" style="display: inline;"> Very young (t $\lesssim$ 10 Myrs) stars possess strong magnetic fields that channel ionized gas from the interiors of their circumstellar discs to the surface of the star. Upon impacting the stellar surface, the shocked gas recombines and emits hydrogen spectral lines. To characterize the density and temperature of the gas within these accretion streams, we measure equivalent widths of Brackett (B… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.06454v2-abstract-full').style.display = 'inline'; document.getElementById('2211.06454v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.06454v2-abstract-full" style="display: none;"> Very young (t $\lesssim$ 10 Myrs) stars possess strong magnetic fields that channel ionized gas from the interiors of their circumstellar discs to the surface of the star. Upon impacting the stellar surface, the shocked gas recombines and emits hydrogen spectral lines. To characterize the density and temperature of the gas within these accretion streams, we measure equivalent widths of Brackett (Br) 11-20 emission lines detected in 1101 APOGEE spectra of 326 likely pre-main sequence accretors. For sources with multiple observations, we measure median epoch-to-epoch line strength variations of 10% in Br11 and 20% in Br20. We also fit the measured line ratios to predictions of radiative transfer models by Kwan & Fischer. We find characteristic best-fit electron densities of $n_e$ = 10$^{11} - 10^{12}$ cm$^{-3}$, and excitation temperatures that are inversely correlated with electron density (from T$\sim$5000 K for $n_e \sim 10^{12}$ cm$^{-3}$, to T$\sim$12500 K at $n_e \sim 10^{11}$ cm$^{-3}$). These physical parameters are in good agreement with predictions from modelling of accretion streams that account for the hydrodynamics and radiative transfer within the accretion stream. We also present a supplementary catalog of line measurements from 9733 spectra of 4255 Brackett emission line sources in the APOGEE DR17 dataset. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.06454v2-abstract-full').style.display = 'none'; document.getElementById('2211.06454v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 9 figures, accepted to AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.13650">arXiv:2206.13650</a> <span> [<a href="https://arxiv.org/pdf/2206.13650">pdf</a>, <a href="https://arxiv.org/format/2206.13650">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac7ce5">10.3847/1538-3881/ac7ce5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Open Cluster Chemical Abundances and Mapping Survey: VI. Galactic Chemical Gradient Analysis from APOGEE DR17 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Myers%2C+N">Natalie Myers</a>, <a href="/search/astro-ph?searchtype=author&query=Donor%2C+J">John Donor</a>, <a href="/search/astro-ph?searchtype=author&query=Spoo%2C+T">Taylor Spoo</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P+M">Peter M. Frinchaboy</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Price-Whelan%2C+A+M">Adrian M. Price-Whelan</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Zasowski%2C+G">Gail Zasowski</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Connell%2C+J">Julia O'Connell</a>, <a href="/search/astro-ph?searchtype=author&query=Ray%2C+A+E">Amy E. Ray</a>, <a href="/search/astro-ph?searchtype=author&query=Bizyaev%2C+D">Dmitry Bizyaev</a>, <a href="/search/astro-ph?searchtype=author&query=Chiappini%2C+C">Cristina Chiappini</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Hern%C3%A1ndez%2C+D+A">D. A. Garc铆a-Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B6nsson%2C+H">Henrik J枚nsson</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Longa-Pe%C3%B1a%2C+P">Pen茅lope Longa-Pe帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Minchev%2C+I">Ivan Minchev</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">A. Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.13650v1-abstract-short" style="display: inline;"> The goal of the Open Cluster Chemical Abundances and Mapping (OCCAM) survey is to constrain key Galactic dynamic and chemical evolution parameters by the construction and analysis of a large, comprehensive, uniform data set of infrared spectra for stars in hundreds of open clusters. This sixth contribution from the OCCAM survey presents analysis of SDSS/APOGEE Data Release 17 (DR17) results for a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.13650v1-abstract-full').style.display = 'inline'; document.getElementById('2206.13650v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.13650v1-abstract-full" style="display: none;"> The goal of the Open Cluster Chemical Abundances and Mapping (OCCAM) survey is to constrain key Galactic dynamic and chemical evolution parameters by the construction and analysis of a large, comprehensive, uniform data set of infrared spectra for stars in hundreds of open clusters. This sixth contribution from the OCCAM survey presents analysis of SDSS/APOGEE Data Release 17 (DR17) results for a sample of stars in 150 open clusters, 94 of which we designate to be "high quality'' based on the appearance of their color-magnitude diagram. We find the APOGEE DR17-derived [Fe/H] values to be in good agreement with those from previous high resolution spectroscopic open cluster abundance studies. Using a subset of the high quality sample, the Galactic abundance gradients were measured for 16 chemical elements, including [Fe/H], for both Galactocentric radius ($R_{GC}$) and guiding center radius ($R_{Guide}$). We find an overall Galactic [Fe/H] vs $R_{GC}$ gradient of $-0.073 \pm 0.002$ dex/kpc over the range of $6 < R_{GC} < 11.5$ kpc, and a similar gradient is found for [Fe/H] versus $R_{Guide}$. Significant Galactic abundance gradients are also noted for O, Mg, S, Ca, Mn, Na, Al, K and Ce. Our large sample additionally allows us to explore the evolution of the gradients in four age bins for the remaining 15 elements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.13650v1-abstract-full').style.display = 'none'; document.getElementById('2206.13650v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 14 Figures, Astronomical Journal Accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.10327">arXiv:2204.10327</a> <span> [<a href="https://arxiv.org/pdf/2204.10327">pdf</a>, <a href="https://arxiv.org/format/2204.10327">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac1151">10.1093/mnras/stac1151 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Milky Way tomography with APOGEE: intrinsic density distribution and structure of mono-abundance populations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lian%2C+J">Jianhui Lian</a>, <a href="/search/astro-ph?searchtype=author&query=Zasowski%2C+G">Gail Zasowski</a>, <a href="/search/astro-ph?searchtype=author&query=Mackereth%2C+T">Ted Mackereth</a>, <a href="/search/astro-ph?searchtype=author&query=Imig%2C+J">Julie Imig</a>, <a href="/search/astro-ph?searchtype=author&query=Holtzman%2C+J+A">Jon A. Holtzman</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Bird%2C+J+C">Jonathan C. Bird</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Horta%2C+D">Danny Horta</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">Karen L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">A. Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.10327v1-abstract-short" style="display: inline;"> The spatial distribution of mono-abundance populations (MAPs, selected in [Fe/H] and [Mg/Fe]) reflect the chemical and structural evolution in a galaxy and impose strong constraints on galaxy formation models. In this paper, we use APOGEE data to derive the intrinsic density distribution of MAPs in the Milky Way, after carefully considering the survey selection function. We find that a single expo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.10327v1-abstract-full').style.display = 'inline'; document.getElementById('2204.10327v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.10327v1-abstract-full" style="display: none;"> The spatial distribution of mono-abundance populations (MAPs, selected in [Fe/H] and [Mg/Fe]) reflect the chemical and structural evolution in a galaxy and impose strong constraints on galaxy formation models. In this paper, we use APOGEE data to derive the intrinsic density distribution of MAPs in the Milky Way, after carefully considering the survey selection function. We find that a single exponential profile is not a sufficient description of the Milky Way's disc. Both the individual MAPs and the integrated disc exhibit a broken radial density distribution; densities are relatively constant with radius in the inner Galaxy and rapidly decrease beyond the break radius. We fit the intrinsic density distribution as a function of radius and vertical height with a 2D density model that considers both a broken radial profile and radial variation of scale height (i.e., flaring). There is a large variety of structural parameters between different MAPs, indicative of strong structure evolution of the Milky Way. One surprising result is that high-$伪$ MAPs show the strongest flaring. The young, solar-abundance MAPs present the shortest scale height and least flaring, suggesting recent and ongoing star formation confined to the disc plane. Finally we derive the intrinsic density distribution and corresponding structural parameters of the chemically defined thin and thick discs. The chemical thick and thin discs have local surface mass densities of 5.62$\pm$0.08 and 15.69$\pm$0.32 ${\rm M_{\odot} pc^{-2}}$, respectively, suggesting a massive thick disc with a local surface mass density ratio between thick to thin disc of 36%. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.10327v1-abstract-full').style.display = 'none'; document.getElementById('2204.10327v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 17 figures, accepted to publish in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.14538">arXiv:2203.14538</a> <span> [<a href="https://arxiv.org/pdf/2203.14538">pdf</a>, <a href="https://arxiv.org/format/2203.14538">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac5f49">10.3847/1538-3881/ac5f49 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Zeta-Payne: a fully automated spectrum analysis algorithm for the Milky Way Mapper program of the SDSS-V survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Straumit%2C+I">Ilya Straumit</a>, <a href="/search/astro-ph?searchtype=author&query=Tkachenko%2C+A">Andrew Tkachenko</a>, <a href="/search/astro-ph?searchtype=author&query=Gebruers%2C+S">Sarah Gebruers</a>, <a href="/search/astro-ph?searchtype=author&query=Audenaert%2C+J">Jeroen Audenaert</a>, <a href="/search/astro-ph?searchtype=author&query=Xiang%2C+M">Maosheng Xiang</a>, <a href="/search/astro-ph?searchtype=author&query=Zari%2C+E">Eleonora Zari</a>, <a href="/search/astro-ph?searchtype=author&query=Aerts%2C+C">Conny Aerts</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J+A">Jennifer A. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Kollmeier%2C+J+A">Juna A. Kollmeier</a>, <a href="/search/astro-ph?searchtype=author&query=Rix%2C+H">Hans-Walter Rix</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Saders%2C+J+L">Jennifer L. Van Saders</a>, <a href="/search/astro-ph?searchtype=author&query=Teske%2C+J">Johanna Teske</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Ting%2C+Y">Yuan-Sen Ting</a>, <a href="/search/astro-ph?searchtype=author&query=Rom%C3%A1n-Z%C3%BA%C3%B1iga%2C+C+G">Carlos G. Rom谩n-Z煤帽iga</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.14538v1-abstract-short" style="display: inline;"> The Sloan Digital Sky Survey has recently initiated its 5th survey generation (SDSS-V), with a central focus on stellar spectroscopy. In particular, SDSS-V Milky Way Mapper program will deliver multi-epoch optical and near-infrared spectra for more than 5 million stars across the entire sky, covering a large range in stellar mass, surface temperature, evolutionary stage, and age. About 10% of thos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.14538v1-abstract-full').style.display = 'inline'; document.getElementById('2203.14538v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.14538v1-abstract-full" style="display: none;"> The Sloan Digital Sky Survey has recently initiated its 5th survey generation (SDSS-V), with a central focus on stellar spectroscopy. In particular, SDSS-V Milky Way Mapper program will deliver multi-epoch optical and near-infrared spectra for more than 5 million stars across the entire sky, covering a large range in stellar mass, surface temperature, evolutionary stage, and age. About 10% of those spectra will be of hot stars of OBAF spectral types, for whose analysis no established survey pipelines exist. Here we present the spectral analysis algorithm, Zeta-Payne, developed specifically to obtain stellar labels from SDSS-V spectra of stars with these spectral types and drawing on machine learning tools. We provide details of the algorithm training, its test on artificial spectra, and its validation on two control samples of real stars. Analysis with Zeta-Payne leads to only modest internal uncertainties in the near-IR with APOGEE (optical with BOSS): 3-10% (1-2%) for Teff, 5-30% (5-25%) for v*sin(i), 1.7-6.3 km/s(0.7-2.2 km/s) for RV, $<0.1$ dex ($<0.05$ dex) for log(g), and 0.4-0.5 dex (0.1 dex) for [M/H] of the star, respectively. We find a good agreement between atmospheric parameters of OBAF-type stars when inferred from their high- and low-resolution optical spectra. For most stellar labels the APOGEE spectra are (far) less informative than the BOSS spectra of these stars, while log(g), v*sin(i), and [M/H] are in most cases too uncertain for meaningful astrophysical interpretation. This makes BOSS low-resolution optical spectra better for stellar labels of OBAF-type stars, unless the latter are subject to high levels of extinction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.14538v1-abstract-full').style.display = 'none'; document.getElementById('2203.14538v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 12 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.05463">arXiv:2203.05463</a> <span> [<a href="https://arxiv.org/pdf/2203.05463">pdf</a>, <a href="https://arxiv.org/format/2203.05463">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac5d53">10.3847/1538-3881/ac5d53 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Open Cluster Chemical Abundances and Mapping Survey: VII. APOGEE DR17 [C/N]-Age Calibration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spoo%2C+T">Taylor Spoo</a>, <a href="/search/astro-ph?searchtype=author&query=Tayar%2C+J">Jamie Tayar</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P+M">Peter M. Frinchaboy</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Myers%2C+N">Natalie Myers</a>, <a href="/search/astro-ph?searchtype=author&query=Donor%2C+J">John Donor</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Bizyaev%2C+D">Dmitry Bizyaev</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Hernandez%2C+D+A">D. A. Garcia-Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Jonsson%2C+H">Henrik Jonsson</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+K">Kaike Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Longa-Pena%2C+P">Penelope Longa-Pena</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">A. Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.05463v1-abstract-short" style="display: inline;"> Large scale surveys open the possibility to investigate Galactic evolution both chemically and kinematically, however, reliable stellar ages remain a major challenge. Detailed chemical information provided by high-resolution spectroscopic surveys of the stars in clusters can be used as a means to calibrate recently developed chemical tools for age-dating field stars. Using data from the Open Clust… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.05463v1-abstract-full').style.display = 'inline'; document.getElementById('2203.05463v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.05463v1-abstract-full" style="display: none;"> Large scale surveys open the possibility to investigate Galactic evolution both chemically and kinematically, however, reliable stellar ages remain a major challenge. Detailed chemical information provided by high-resolution spectroscopic surveys of the stars in clusters can be used as a means to calibrate recently developed chemical tools for age-dating field stars. Using data from the Open Cluster Abundances and Mapping (OCCAM) survey, based on the SDSS/APOGEE-2 survey, we derive a new empirical relationship between open cluster stellar ages and the carbon-to-nitrogen ([C/N]) abundance ratios for evolved stars, primarily those on the red giant branch. With this calibration, [C/N] can be used a chemical clock for evolved field stars to investigate the formation and evolution of different parts of our Galaxy. We explore how mixing effects at different stellar evolutionary phases, like the red clump, affect the derived calibration. We have established the [C/N]-age calibration for APOGEE DR17 giant star abundances to be $\log[Age({\rm yr})]_{\rm DR17} = 10.14 \, (\pm 0.08) + 2.23\,(\pm 0.19) \, {\rm [C/N]}$, usable for $8.62 \leq \log(Age[{\rm yr}]) \leq 9.82$, derived from a uniform sample of 49 clusters observed as part of APOGEE DR17 applicable primarily to metal-rich, thin and thick disk giant stars. This measured [C/N]-age APOGEE DR17 calibration is also shown to be consistent with astereoseismic ages derived from Kepler photometry. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.05463v1-abstract-full').style.display = 'none'; document.getElementById('2203.05463v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 6 figures, accepted Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.03661">arXiv:2201.03661</a> <span> [<a href="https://arxiv.org/pdf/2201.03661">pdf</a>, <a href="https://arxiv.org/format/2201.03661">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac4de7">10.3847/1538-3881/ac4de7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> APOGEE Net: An expanded spectral model of both low mass and high mass stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sprague%2C+D">Dani Sprague</a>, <a href="/search/astro-ph?searchtype=author&query=Culhane%2C+C">Connor Culhane</a>, <a href="/search/astro-ph?searchtype=author&query=Kounkel%2C+M">Marina Kounkel</a>, <a href="/search/astro-ph?searchtype=author&query=Olney%2C+R">Richard Olney</a>, <a href="/search/astro-ph?searchtype=author&query=Covey%2C+K+R">K. R. Covey</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchinson%2C+B">Brian Hutchinson</a>, <a href="/search/astro-ph?searchtype=author&query=Lingg%2C+R">Ryan Lingg</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Rom%C3%A1n-Z%C3%BA%C3%B1iga%2C+C+G">Carlos G. Rom谩n-Z煤帽iga</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D">David Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">Jura Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Stutz%2C+A">Amelia Stutz</a>, <a href="/search/astro-ph?searchtype=author&query=Stringfellow%2C+G+S">Guy S. Stringfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez%2C+K+P">Karla Pe帽a Ram铆rez</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez-Preciado%2C+V">Valeria Ram铆rez-Preciado</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">Jes煤s Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J+S">Jinyoung Serena Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.03661v2-abstract-short" style="display: inline;"> We train a convolutional neural network, APOGEE Net, to predict $T_\mathrm{eff}$, $\log g$, and, for some stars, [Fe/H], based on the APOGEE spectra. This is the first pipeline adapted for these data that is capable of estimating these parameters in a self-consistent manner not only for low mass stars, (such as main sequence dwarfs, pre-main sequence stars, and red giants), but also high mass star… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03661v2-abstract-full').style.display = 'inline'; document.getElementById('2201.03661v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.03661v2-abstract-full" style="display: none;"> We train a convolutional neural network, APOGEE Net, to predict $T_\mathrm{eff}$, $\log g$, and, for some stars, [Fe/H], based on the APOGEE spectra. This is the first pipeline adapted for these data that is capable of estimating these parameters in a self-consistent manner not only for low mass stars, (such as main sequence dwarfs, pre-main sequence stars, and red giants), but also high mass stars with $T_\mathrm{eff}$ in excess of 50,000 K, including hot dwarfs and blue supergiants. The catalog of ~650,000 stars presented in this paper allows for a detailed investigation of the star forming history of not just the Milky Way, but also of the Magellanic clouds, as different type of objects tracing different parts of these galaxies can be more cleanly selected through their distinct placement in $T_\mathrm{eff}$-$\log g$ parameter space than in previous APOGEE catalogs produced through different pipelines. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03661v2-abstract-full').style.display = 'none'; document.getElementById('2201.03661v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 11 figures. Accepted to AJ. Data are available through https://www.sdss.org/dr17/data_access/value-added-catalogs/?vac_id=apogee-net:-a-unified-spectral-model Code is available through https://github.com/hutchresearch/ApogeeNet2</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.02026">arXiv:2112.02026</a> <span> [<a href="https://arxiv.org/pdf/2112.02026">pdf</a>, <a href="https://arxiv.org/format/2112.02026">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac4414">10.3847/1538-4365/ac4414 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Seventeenth Data Release of the Sloan Digital Sky Surveys: Complete Release of MaNGA, MaStar and APOGEE-2 Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Accetta%2C+K">Katherine Accetta</a>, <a href="/search/astro-ph?searchtype=author&query=Aerts%2C+C">Conny Aerts</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre%2C+V+S">Victor Silva Aguirre</a>, <a href="/search/astro-ph?searchtype=author&query=Ahumada%2C+R">Romina Ahumada</a>, <a href="/search/astro-ph?searchtype=author&query=Ajgaonkar%2C+N">Nikhil Ajgaonkar</a>, <a href="/search/astro-ph?searchtype=author&query=Ak%2C+N+F">N. Filiz Ak</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">Shadab Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+A">Andres Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Anders%2C+F">Friedrich Anders</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S+F">Scott F. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+B+H">Brett H. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Anguiano%2C+B">Borja Anguiano</a>, <a href="/search/astro-ph?searchtype=author&query=Aquino-Ortiz%2C+E">Erik Aquino-Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Aragon-Salamanca%2C+A">Alfonso Aragon-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Argudo-Fernandez%2C+M">Maria Argudo-Fernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Ata%2C+M">Metin Ata</a>, <a href="/search/astro-ph?searchtype=author&query=Aubert%2C+M">Marie Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Avila-Reese%2C+V">Vladimir Avila-Reese</a>, <a href="/search/astro-ph?searchtype=author&query=Badenes%2C+C">Carles Badenes</a>, <a href="/search/astro-ph?searchtype=author&query=Barba%2C+R+H">Rodolfo H. Barba</a>, <a href="/search/astro-ph?searchtype=author&query=Barger%2C+K">Kat Barger</a>, <a href="/search/astro-ph?searchtype=author&query=Barrera-Ballesteros%2C+J+K">Jorge K. Barrera-Ballesteros</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a> , et al. (316 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.02026v2-abstract-short" style="display: inline;"> This paper documents the seventeenth data release (DR17) from the Sloan Digital Sky Surveys; the fifth and final release from the fourth phase (SDSS-IV). DR17 contains the complete release of the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey, which reached its goal of surveying over 10,000 nearby galaxies. The complete release of the MaNGA Stellar Library (MaStar) accompanies… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.02026v2-abstract-full').style.display = 'inline'; document.getElementById('2112.02026v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.02026v2-abstract-full" style="display: none;"> This paper documents the seventeenth data release (DR17) from the Sloan Digital Sky Surveys; the fifth and final release from the fourth phase (SDSS-IV). DR17 contains the complete release of the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey, which reached its goal of surveying over 10,000 nearby galaxies. The complete release of the MaNGA Stellar Library (MaStar) accompanies this data, providing observations of almost 30,000 stars through the MaNGA instrument during bright time. DR17 also contains the complete release of the Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2) survey which publicly releases infra-red spectra of over 650,000 stars. The main sample from the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), as well as the sub-survey Time Domain Spectroscopic Survey (TDSS) data were fully released in DR16. New single-fiber optical spectroscopy released in DR17 is from the SPectroscipic IDentification of ERosita Survey (SPIDERS) sub-survey and the eBOSS-RM program. Along with the primary data sets, DR17 includes 25 new or updated Value Added Catalogs (VACs). This paper concludes the release of SDSS-IV survey data. SDSS continues into its fifth phase with observations already underway for the Milky Way Mapper (MWM), Local Volume Mapper (LVM) and Black Hole Mapper (BHM) surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.02026v2-abstract-full').style.display = 'none'; document.getElementById('2112.02026v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">40 pages, 8 figures, 6 tables. In press at ApJSS (arxiv v2 corrects some minor typos and updates references)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.06431">arXiv:2110.06431</a> <span> [<a href="https://arxiv.org/pdf/2110.06431">pdf</a>, <a href="https://arxiv.org/format/2110.06431">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac300a">10.3847/1538-4357/ac300a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar Rotation of T Tauri stars in the Orion Star-Forming Complex </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Serna%2C+J">Javier Serna</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">Jes煤s Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Kounkel%2C+M">Marina Kounkel</a>, <a href="/search/astro-ph?searchtype=author&query=Manzo-Mart%C3%ADnez%2C+E">Ezequiel Manzo-Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Rom%C3%A1n-Zu%C3%B1iga%2C+C+G">Carlos G. Rom谩n-Zu帽iga</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+M+G">Maria Gracia Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Pinz%C3%B3n%2C+G">Giovanni Pinz贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Calvet%2C+N">Nuria Calvet</a>, <a href="/search/astro-ph?searchtype=author&query=Brice%C3%B1o%2C+C">Cesar Brice帽o</a>, <a href="/search/astro-ph?searchtype=author&query=Tapia%2C+M">Mauricio Tapia</a>, <a href="/search/astro-ph?searchtype=author&query=Su%C3%A1rez%2C+G">Genaro Su谩rez</a>, <a href="/search/astro-ph?searchtype=author&query=Ramirez%2C+K+P">Karla Pe帽a Ramirez</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Covey%2C+K">Kevin Covey</a>, <a href="/search/astro-ph?searchtype=author&query=Vargas-Gonz%C3%A1lez%2C+J">Jaime Vargas-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 Gregorio Fern谩ndez-Trincado</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.06431v1-abstract-short" style="display: inline;"> We present a large-scale study of stellar rotation for T Tauri stars in the Orion Star-Forming Complex. We use the projected rotational velocity ($v\sin(i)$) estimations reported by the APOGEE-2 collaboration as well as individual masses and ages derived from the position of the stars in the HR diagram, considering Gaia-EDR3 parallaxes and photometry plus diverse evolutionary models. We find an em… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.06431v1-abstract-full').style.display = 'inline'; document.getElementById('2110.06431v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.06431v1-abstract-full" style="display: none;"> We present a large-scale study of stellar rotation for T Tauri stars in the Orion Star-Forming Complex. We use the projected rotational velocity ($v\sin(i)$) estimations reported by the APOGEE-2 collaboration as well as individual masses and ages derived from the position of the stars in the HR diagram, considering Gaia-EDR3 parallaxes and photometry plus diverse evolutionary models. We find an empirical trend for $v\sin(i)$ decreasing with age for low-mass stars ($0.4 M_{\odot} < M_{\ast} < 1.2 M_{\odot}$). Our results support the existence of a mechanism linking $v\sin(i)$ to the presence of accreting protoplanetary disks, responsible for regulating stellar rotation in timescales of about 6 Myr, which is the timescale in which most of the T Tauri stars lose their inner disk. Our results provide important constraints to models of rotation in the early phases of evolution of young stars and their disks. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.06431v1-abstract-full').style.display = 'none'; document.getElementById('2110.06431v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 10 figures, Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.05130">arXiv:2109.05130</a> <span> [<a href="https://arxiv.org/pdf/2109.05130">pdf</a>, <a href="https://arxiv.org/format/2109.05130">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac25f9">10.3847/1538-4357/ac25f9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> APOGEE Chemical Abundance Patterns of the Massive Milky Way Satellites </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Hayes%2C+C+R">Christian R. Hayes</a>, <a href="/search/astro-ph?searchtype=author&query=Lian%2C+J">Jianhui Lian</a>, <a href="/search/astro-ph?searchtype=author&query=Weinberg%2C+D+H">David H. Weinberg</a>, <a href="/search/astro-ph?searchtype=author&query=Zasowski%2C+G">Gail Zasowski</a>, <a href="/search/astro-ph?searchtype=author&query=Horta%2C+D">Danny Horta</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachael Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Feuillet%2C+D+K">Diane K. Feuillet</a>, <a href="/search/astro-ph?searchtype=author&query=Garro%2C+E+R">Elisa R. Garro</a>, <a href="/search/astro-ph?searchtype=author&query=Gallart%2C+C">Carme Gallart</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+V+V">Verne V. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Holtzman%2C+J+A">Jon A. Holtzman</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Lacerna%2C+I">Ivan Lacerna</a>, <a href="/search/astro-ph?searchtype=author&query=Shetrone%2C+M">Matthew Shetrone</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B6nsson%2C+H">Henrik J枚nsson</a>, <a href="/search/astro-ph?searchtype=author&query=Cioni%2C+M+L">Maria-Rosa L. Cioni</a>, <a href="/search/astro-ph?searchtype=author&query=Fillingham%2C+S+P">Sean P. Fillingham</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=O%C4%86onnell%2C+R">Robert O膯onnell</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+R+R">Ricardo R. Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Schiavon%2C+R">Ricardo Schiavon</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+A">Andres Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Anguiano%2C+B">Borja Anguiano</a> , et al. (20 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.05130v2-abstract-short" style="display: inline;"> The SDSS-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey has obtained high-resolution spectra for thousands of red giant stars distributed among the massive satellite galaxies of the Milky Way (MW): the Large and Small Magellanic Clouds (LMC/SMC), the Sagittarius Dwarf (Sgr), Fornax (Fnx), and the now fully disrupted \emph{Gaia} Sausage/Enceladus (GSE) system. We present… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.05130v2-abstract-full').style.display = 'inline'; document.getElementById('2109.05130v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.05130v2-abstract-full" style="display: none;"> The SDSS-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey has obtained high-resolution spectra for thousands of red giant stars distributed among the massive satellite galaxies of the Milky Way (MW): the Large and Small Magellanic Clouds (LMC/SMC), the Sagittarius Dwarf (Sgr), Fornax (Fnx), and the now fully disrupted \emph{Gaia} Sausage/Enceladus (GSE) system. We present and analyze the APOGEE chemical abundance patterns of each galaxy to draw robust conclusions about their star formation histories, by quantifying the relative abundance trends of multiple elements (C, N, O, Mg, Al, Si, Ca, Fe, Ni, and Ce), as well as by fitting chemical evolution models to the [$伪$/Fe]-[Fe/H] abundance plane for each galaxy. Results show that the chemical signatures of the starburst in the MCs observed by Nidever et al. in the $伪$-element abundances extend to C+N, Al, and Ni, with the major burst in the SMC occurring some 3-4 Gyr before the burst in the LMC. We find that Sgr and Fnx also exhibit chemical abundance patterns suggestive of secondary star formation epochs, but these events were weaker and earlier ($\sim$~5-7 Gyr ago) than those observed in the MCs. There is no chemical evidence of a second starburst in GSE, but this galaxy shows the strongest initial star formation as compared to the other four galaxies. All dwarf galaxies had greater relative contributions of AGB stars to their enrichment than the MW. Comparing and contrasting these chemical patterns highlight the importance of galaxy environment on its chemical evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.05130v2-abstract-full').style.display = 'none'; document.getElementById('2109.05130v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages, 21 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.11908">arXiv:2108.11908</a> <span> [<a href="https://arxiv.org/pdf/2108.11908">pdf</a>, <a href="https://arxiv.org/format/2108.11908">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac2cbc">10.3847/1538-3881/ac2cbc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Final Targeting Strategy for the SDSS-IV APOGEE-2S Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Santana%2C+F+A">Felipe A. Santana</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Covey%2C+K+R">Kevin R. Covey</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Connell%2C+J+E">Julia E. O'Connell</a>, <a href="/search/astro-ph?searchtype=author&query=Longa-Pe%C3%B1a%2C+P">Pen茅lope Longa-Pe帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R">Roger Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Hayes%2C+C+R">Christian R. Hayes</a>, <a href="/search/astro-ph?searchtype=author&query=Zasowski%2C+G">Gail Zasowski</a>, <a href="/search/astro-ph?searchtype=author&query=Sobeck%2C+J+S">Jennifer S. Sobeck</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Chojnowski%2C+S+D">S. D. Chojnowski</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lee%2C+N">Nathan De Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Oelkers%2C+R+J">Ryan J. Oelkers</a>, <a href="/search/astro-ph?searchtype=author&query=Stringfellow%2C+G+S">Guy S. Stringfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+A">Andr茅s Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Anguiano%2C+B">Borja Anguiano</a>, <a href="/search/astro-ph?searchtype=author&query=Donor%2C+J">John Donor</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P+M">Peter M. Frinchaboy</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J+A">Jennifer A. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Kollmeier%2C+J+A">Juna A. Kollmeier</a>, <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D+L">David L. Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Price-Whelan%2C+A+M">Adrian. M. Price-Whelan</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+A">Alvaro Rojas-Arriagada</a> , et al. (21 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.11908v1-abstract-short" style="display: inline;"> APOGEE is a high-resolution (R sim 22,000), near-infrared, multi-epoch, spectroscopic survey of the Milky Way. The second generation of the APOGEE project, APOGEE-2, includes an expansion of the survey to the Southern Hemisphere called APOGEE-2S. This expansion enabled APOGEE to perform a fully panoramic mapping of all the main regions of the Milky Way; in particular, by operating in the H-band, A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.11908v1-abstract-full').style.display = 'inline'; document.getElementById('2108.11908v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.11908v1-abstract-full" style="display: none;"> APOGEE is a high-resolution (R sim 22,000), near-infrared, multi-epoch, spectroscopic survey of the Milky Way. The second generation of the APOGEE project, APOGEE-2, includes an expansion of the survey to the Southern Hemisphere called APOGEE-2S. This expansion enabled APOGEE to perform a fully panoramic mapping of all the main regions of the Milky Way; in particular, by operating in the H-band, APOGEE is uniquely able to probe the dust-hidden inner regions of the Milky Way that are best accessed from the Southern Hemisphere. In this paper we present the targeting strategy of APOGEE-2S, with special attention to documenting modifications to the original, previously published plan. The motivation for these changes is explained as well as an assessment of their effectiveness in achieving their intended scientific objective. In anticipation of this being the last paper detailing APOGEE targeting, we present an accounting of all such information complete through the end of the APOGEE-2S project; this includes several main survey programs dedicated to exploration of major stellar populations and regions of the Milky Way, as well as a full list of programs contributing to the APOGEE database through allocations of observing time by the Chilean National Time Allocation Committee (CNTAC) and the Carnegie Institution for Science (CIS). This work was presented along with a companion article, R. Beaton et al. (submitted; AAS29028), presenting the final target selection strategy adopted for APOGEE-2 in the Northern Hemisphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.11908v1-abstract-full').style.display = 'none'; document.getElementById('2108.11908v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">43 pages; 5 figures; 6 Tables; 1 Appendix; Submitted to Journal and Under Review; Posting to accompany papers using the SDSS-IV/APOGEE-2 Data Release 17 scheduled for December 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.11907">arXiv:2108.11907</a> <span> [<a href="https://arxiv.org/pdf/2108.11907">pdf</a>, <a href="https://arxiv.org/format/2108.11907">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac260c">10.3847/1538-3881/ac260c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Final Targeting Strategy for the SDSS-IV APOGEE-2N Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Oelkers%2C+R+J">Ryan J. Oelkers</a>, <a href="/search/astro-ph?searchtype=author&query=Hayes%2C+C+R">Christian R. Hayes</a>, <a href="/search/astro-ph?searchtype=author&query=Covey%2C+K+R">Kevin R. Covey</a>, <a href="/search/astro-ph?searchtype=author&query=Chojnowski%2C+S+D">S. D. Chojnowski</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lee%2C+N">Nathan De Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Sobeck%2C+J+S">Jennifer S. Sobeck</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R">Roger Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Trincado%2C+J">Jose Fernandez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Longa-Pena%2C+P">Penelope Longa-Pena</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Connell%2C+J+E">Julia E. O'Connell</a>, <a href="/search/astro-ph?searchtype=author&query=Santana%2C+F+A">Felipe A. Santana</a>, <a href="/search/astro-ph?searchtype=author&query=Stringfellow%2C+G+S">Guy S. Stringfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Zasowski%2C+G">Gail Zasowski</a>, <a href="/search/astro-ph?searchtype=author&query=Aerts%2C+C">Conny Aerts</a>, <a href="/search/astro-ph?searchtype=author&query=Anguiano%2C+B">Borja Anguiano</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+C">Chad Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Canas%2C+C+I">Caleb I. Canas</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Fleming%2C+J+D+S+W">John Donor Scott W. Fleming</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P+M">Peter M. Frinchaboy</a>, <a href="/search/astro-ph?searchtype=author&query=Feuillet%2C+D">Diane Feuillet</a>, <a href="/search/astro-ph?searchtype=author&query=Harding%2C+P">Paul Harding</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a> , et al. (35 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.11907v1-abstract-short" style="display: inline;"> APOGEE-2 is a dual-hemisphere, near-infrared (NIR), spectroscopic survey with the goal of producing a chemo-dynamical mapping of the Milky Way Galaxy. The targeting for APOGEE-2 is complex and has evolved with time. In this paper, we present the updates and additions to the initial targeting strategy for APOGEE-2N presented in Zasowski et al. (2017). These modifications come in two implementation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.11907v1-abstract-full').style.display = 'inline'; document.getElementById('2108.11907v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.11907v1-abstract-full" style="display: none;"> APOGEE-2 is a dual-hemisphere, near-infrared (NIR), spectroscopic survey with the goal of producing a chemo-dynamical mapping of the Milky Way Galaxy. The targeting for APOGEE-2 is complex and has evolved with time. In this paper, we present the updates and additions to the initial targeting strategy for APOGEE-2N presented in Zasowski et al. (2017). These modifications come in two implementation modes: (i) "Ancillary Science Programs" competitively awarded to SDSS-IV PIs through proposal calls in 2015 and 2017 for the pursuit of new scientific avenues outside the main survey, and (ii) an effective 1.5-year expansion of the survey, known as the Bright Time Extension, made possible through accrued efficiency gains over the first years of the APOGEE-2N project. For the 23 distinct ancillary programs, we provide descriptions of the scientific aims, target selection, and how to identify these targets within the APOGEE-2 sample. The Bright Time Extension permitted changes to the main survey strategy, the inclusion of new programs in response to scientific discoveries or to exploit major new datasets not available at the outset of the survey design, and expansions of existing programs to enhance their scientific success and reach. After describing the motivations, implementation, and assessment of these programs, we also leave a summary of lessons learned from nearly a decade of APOGEE-1 and APOGEE-2 survey operations. A companion paper, Santana et al. (submitted), provides a complementary presentation of targeting modifications relevant to APOGEE-2 operations in the Southern Hemisphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.11907v1-abstract-full').style.display = 'none'; document.getElementById('2108.11907v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">59 pages; 11 Figures; 7 Tables; 2 Appendices; Submitted to Journal and Under Review; Posting to accompany papers using the SDSS-IV/APOGEE-2 Data Release 17 scheduled for December 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.12884">arXiv:2105.12884</a> <span> [<a href="https://arxiv.org/pdf/2105.12884">pdf</a>, <a href="https://arxiv.org/format/2105.12884">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac04ae">10.3847/1538-3881/ac04ae <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Understanding the angular momentum evolution of T Tauri and Herbig Ae/Be stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pinz%C3%B3n%2C+G">Giovanni Pinz贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">Jes煤s Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Serna%2C+J">Javier Serna</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+A">Alexandra Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Manzo-Mart%C3%ADnez%2C+E">Ezequiel Manzo-Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Rom%C3%A1n-Z%C3%BA%C3%B1iga%2C+C+G">Carlos G. Rom谩n-Z煤帽iga</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+M+G">Maria Gracia Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez-V%C3%A9lez%2C+J">Julio Ram铆rez-V茅lez</a>, <a href="/search/astro-ph?searchtype=author&query=Osorio%2C+Y">Yeisson Osorio</a>, <a href="/search/astro-ph?searchtype=author&query=Avenda%C3%B1o%2C+R">Ronald Avenda帽o</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.12884v1-abstract-short" style="display: inline;"> We investigate a sample of 6 Herbig Ae/Be stars belonging to the Orion OB1 association, as well as 73 low mass objects, members of the $蟽$ Orionis cluster, in order to explore the angular momentum evolution at early stages of evolution, and its possible connection with main-sequence Ap/Bp magnetic stars. Using FIES and HECTOCHELLE spectra, we obtain projected rotational velocities through two inde… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.12884v1-abstract-full').style.display = 'inline'; document.getElementById('2105.12884v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.12884v1-abstract-full" style="display: none;"> We investigate a sample of 6 Herbig Ae/Be stars belonging to the Orion OB1 association, as well as 73 low mass objects, members of the $蟽$ Orionis cluster, in order to explore the angular momentum evolution at early stages of evolution, and its possible connection with main-sequence Ap/Bp magnetic stars. Using FIES and HECTOCHELLE spectra, we obtain projected rotational velocities through two independent methods. Individual masses, radii, and ages were computed using evolutionary models, distance, and cluster extinction. Under the assumption that similar physical processes operate in both, T Tauri and Herbig Ae/Be stars, we construct snapshots of the protostar's rotation against mass during the first 10 Myr with the aid of a rotational model that includes a variable disc lifetime, changes in the stellar moment of inertia, a dipolar magnetic field with variable strength, and angular momentum loss through stellar winds powered by accretion. We use these snapshots, as well as the rotational data, to infer a plausible scenario for the angular momentum evolution. We find that magnetic field strengths of a few k$G$ at 3 Myr are required to match the rotational velocities of both groups of stars. Models with masses between 2-3 $M_{\odot}$ display larger angular momentum by a factor of $\sim 3$, in comparison to stars of similar spectral types on the main-sequence. Even though some quantitative estimates on this dramatic decrease with age, for Ap/Bp magnetic main-sequence stars are presented, the results obtained for the angular momentum evolution do not explain their low rotation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.12884v1-abstract-full').style.display = 'none'; document.getElementById('2105.12884v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">39 pages, 18 figures, Accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.12075">arXiv:2104.12075</a> <span> [<a href="https://arxiv.org/pdf/2104.12075">pdf</a>, <a href="https://arxiv.org/ps/2104.12075">ps</a>, <a href="https://arxiv.org/format/2104.12075">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab1208">10.1093/mnras/stab1208 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Homogeneous Analysis of Globular Clusters from the APOGEE Survey with the BACCHUS Code $-$ III. $蠅$ Cen </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=M%C3%A9sz%C3%A1ros%2C+S">Szabolcs M茅sz谩ros</a>, <a href="/search/astro-ph?searchtype=author&query=Masseron%2C+T">Thomas Masseron</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Hern%C3%A1ndez%2C+D+A">D. A. Garc铆a-Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Szigeti%2C+L">L谩szl贸 Szigeti</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Shetrone%2C+M">Matthew Shetrone</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+V+V">Verne V. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Brownstein%2C+J+R">Joel R. Brownstein</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Hayes%2C+C+R">Christian R. Hayes</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B6nsson%2C+H">Henrik J枚nsson</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Munoz%2C+R+R">Ricardo R. Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+O">Olga Zamora</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.12075v1-abstract-short" style="display: inline;"> We study the multiple populations of $蠅$ Cen by using the abundances of Fe, C, N, O, Mg, Al, Si, K, Ca, and Ce from the high-resolution, high signal-to-noise (S/N$>$70) spectra of 982 red giant stars observed by the SDSS-IV/APOGEE-2 survey. We find that the shape of the Al-Mg and N-C anticorrelations changes as a function of metallicity, continuous for the metal-poor groups, but bimodal (or unimod… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.12075v1-abstract-full').style.display = 'inline'; document.getElementById('2104.12075v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.12075v1-abstract-full" style="display: none;"> We study the multiple populations of $蠅$ Cen by using the abundances of Fe, C, N, O, Mg, Al, Si, K, Ca, and Ce from the high-resolution, high signal-to-noise (S/N$>$70) spectra of 982 red giant stars observed by the SDSS-IV/APOGEE-2 survey. We find that the shape of the Al-Mg and N-C anticorrelations changes as a function of metallicity, continuous for the metal-poor groups, but bimodal (or unimodal) at high metallicities. There are four Fe populations, similar to what has been found in previously published investigations, but we find seven populations based on Fe, Al, and Mg abundances. The evolution of Al in $蠅$ Cen is compared to its evolution in the Milky Way and in five representative globular clusters. We find that the distribution of Al in metal-rich stars of $蠅$ Cen closely follows what is observed in the Galaxy. Other $伪-$elements and C, N, O, and Ce are also compared to the Milky Way, and significantly elevated abundances are observed over what is found in the thick disk for almost all elements. However, we also find some stars with high metallicity and low [Al/Fe], suggesting that $蠅$ Cen could be the remnant core of a dwarf galaxy, but the existence of these peculiar stars needs an independent confirmation. We also confirm the increase in the sum of CNO as a function of metallicity previously reported in the literature and find that the [C/N] ratio appears to show opposite correlations between Al-poor and Al-rich stars as a function of metallicity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.12075v1-abstract-full').style.display = 'none'; document.getElementById('2104.12075v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS, 17 pages, 16 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.02200">arXiv:2104.02200</a> <span> [<a href="https://arxiv.org/pdf/2104.02200">pdf</a>, <a href="https://arxiv.org/format/2104.02200">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abf639">10.3847/1538-4357/abf639 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The G 305 Star-forming Region: II. Irregular variable stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Medina%2C+N">N. Medina</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garc%C3%ADa%2C+J">J. Alonso-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Rom%C3%A1n-Z%C3%BA%C3%B1iga%2C+C+G">Carlos G. Rom谩n-Z煤帽iga</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Kounkel%2C+M">Marina Kounkel</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Covey%2C+K+R">K. R. Covey</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%B6rster%2C+F">Francisco F枚rster</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+L">Lucia Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">Jes煤s Hern谩ndez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.02200v1-abstract-short" style="display: inline;"> We present a catalog of 167 newly discovered, irregular variables spanning a $\sim$7 deg${^2}$ area that encompasses the G 305 star-forming complex, one of the most luminous giant H II regions in the Galaxy. We aim to unveil and characterize the young stellar object (YSO) population of the region by analyzing the $K_{\rm s}$-band variability and $JHK_{\rm s}$ infrared colors from the {\it VISTA Va… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.02200v1-abstract-full').style.display = 'inline'; document.getElementById('2104.02200v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.02200v1-abstract-full" style="display: none;"> We present a catalog of 167 newly discovered, irregular variables spanning a $\sim$7 deg${^2}$ area that encompasses the G 305 star-forming complex, one of the most luminous giant H II regions in the Galaxy. We aim to unveil and characterize the young stellar object (YSO) population of the region by analyzing the $K_{\rm s}$-band variability and $JHK_{\rm s}$ infrared colors from the {\it VISTA Variables in the V铆a L谩ctea} (VVV) survey. Additionally, SDSS-IV APOGEE-2 infrared spectra of selected objects are analyzed. The sample show relatively high amplitudes ($0.661<螖K_{\rm S} <3.521$ mag). Most of them resemble sources with outbursts with amplitude $>1$ mag and duration longer than a few days, typically at least a year, known as {\it Eruptive Variables}. About 60% are likely to be Class II/Flat/I objects. This is also confirmed by the spectral index $伪$ when available. From the analysis of APOGEE-2 near-infrared spectra of sources in the region, another 122 stars are classified as YSOs, and displays some infrared variability. The measured effective temperature $T_{\rm eff}$ peak is around 4000K and they are slightly super-solar in metal abundance. The modal radial velocity is approximately $-$41 km/s. Combining available catalogs of YSOs in the region with our data, we investigate the spatial distributions of 700 YSOs. They are clearly concentrated within the central cavity formed by the massive clusters Danks 1 and 2. The calculated surface density for the entire catalog is 0.025 YSOs/pc$^{-2}$, while the central cavity contains 10 times more objects per area (0.238 YSOs/pc$^{-2}$). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.02200v1-abstract-full').style.display = 'none'; document.getElementById('2104.02200v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 13 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> AAS26957R1 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.07488">arXiv:2103.07488</a> <span> [<a href="https://arxiv.org/pdf/2103.07488">pdf</a>, <a href="https://arxiv.org/format/2103.07488">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abee93">10.3847/1538-4357/abee93 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chemodynamically Characterizing the Jhelum Stellar Stream with APOGEE-2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sheffield%2C+A+A">Allyson A. Sheffield</a>, <a href="/search/astro-ph?searchtype=author&query=Subrahimovic%2C+A+Z">Aidan Z. Subrahimovic</a>, <a href="/search/astro-ph?searchtype=author&query=Refat%2C+M">Mohammad Refat</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Hayes%2C+C+R">Christian R. Hayes</a>, <a href="/search/astro-ph?searchtype=author&query=Price-Whelan%2C+A+M">Adrian. M. Price-Whelan</a>, <a href="/search/astro-ph?searchtype=author&query=Horta%2C+D">Danny Horta</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+V+V">Verne V. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Trincado%2C+J+G">Jose G. Fernandez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Sobeck%2C+J+S">Jennifer S. Sobeck</a>, <a href="/search/astro-ph?searchtype=author&query=Munoz%2C+R+R">Ricardo R. Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Hernandez%2C+D+A">D. A. Garcia-Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.07488v1-abstract-short" style="display: inline;"> We present the kinematic and chemical profiles of red giant stars observed by the APOGEE-2 survey in the direction of the Jhelum stellar stream, a Milky Way substructure located in the inner halo of the Milky Way at a distance from the Sun of $\approx$ 13 kpc. From the six APOGEE-2 Jhelum pointings, we isolate stars with log($g$) $<$ 3.5, leaving a sample of 289 red giant stars. From this sample o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.07488v1-abstract-full').style.display = 'inline'; document.getElementById('2103.07488v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.07488v1-abstract-full" style="display: none;"> We present the kinematic and chemical profiles of red giant stars observed by the APOGEE-2 survey in the direction of the Jhelum stellar stream, a Milky Way substructure located in the inner halo of the Milky Way at a distance from the Sun of $\approx$ 13 kpc. From the six APOGEE-2 Jhelum pointings, we isolate stars with log($g$) $<$ 3.5, leaving a sample of 289 red giant stars. From this sample of APOGEE giants, we identified seven stars that are consistent with the astrometric signal from $Gaia$ DR2 for this stream. Of these seven, one falls onto the RGB along the same sequence as the Jhelum stars presented by \cite{ji20}. This new Jhelum member has [Fe/H]=-2.2 and is at the tip of the red giant branch. By selecting high orbital eccentricity, metal-rich stars, we identify red giants in our APOGEE sample that are likely associated with the $Gaia$-Enceladus-Sausage (GES) merger. We compare the abundance profiles of the Jhelum stars and GES stars and find similar trends in $伪$-elements, as expected for low-metallicity populations. However, we find that the orbits for GES and Jhelum stars are not generally consistent with a shared origin. The chemical abundances for the APOGEE Jhelum star and other confirmed members of the stream are similar to stars in known stellar streams and thus are consistent with an accreted dwarf galaxy origin for the progenitor of the stream, although we cannot rule out a globular cluster origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.07488v1-abstract-full').style.display = 'none'; document.getElementById('2103.07488v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.07785">arXiv:2102.07785</a> <span> [<a href="https://arxiv.org/pdf/2102.07785">pdf</a>, <a href="https://arxiv.org/format/2102.07785">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140306">10.1051/0004-6361/202140306 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> APOGEE spectroscopic evidence for chemical anomalies in dwarf galaxies: The case of M~54 and Sagittarius </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">Christian Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">Sandro Villanova</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Bizyaev%2C+D">Dmitry Bizyaev</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.07785v1-abstract-short" style="display: inline;"> We present evidence for globular cluster stellar debris in a dwarf galaxy system (Sagittarius: Sgr) based on an analysis of high-resolution \textit{H}-band spectra from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. We add [N/Fe], [Ti/Fe], and [Ni/Fe] abundance ratios to the existing sample of potential members of M~54; this is the first time that [N/Fe] abundances are… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.07785v1-abstract-full').style.display = 'inline'; document.getElementById('2102.07785v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.07785v1-abstract-full" style="display: none;"> We present evidence for globular cluster stellar debris in a dwarf galaxy system (Sagittarius: Sgr) based on an analysis of high-resolution \textit{H}-band spectra from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. We add [N/Fe], [Ti/Fe], and [Ni/Fe] abundance ratios to the existing sample of potential members of M~54; this is the first time that [N/Fe] abundances are derived for a large number of stars in M~54. Our study reveals the existence of a significant population of nitrogen- (with a large spread, $\gtrsim1$ dex) and aluminum-enriched stars with moderate Mg depletion in the core of the M~54$+$Sagittarius system, which shares the light element anomalies characteristic of second-generation globular cluster stars (GCs), thus tracing the typical phenomenon of multiple stellar populations seen in other Galactic GCs at similar metallicity, confirming earlier results based on the Na-O anti-correlation. We further show that most of the stars in M~54 exhibit different chemical - patterns evidently not present in Sgr field stars. Furthermore, we report the serendipitous discovery of a nitrogen-enhanced extra-tidal star with GC second-generation-like chemical patterns for which both chemical and kinematic evidence is commensurate with the hypothesis that the star has been ejected from M~54. Our findings support the existence of chemical anomalies associated with likely tidally shredded GCs in dwarf galaxies in the Local Group and motivate future searches for such bonafide stars along other known Milky Way streams. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.07785v1-abstract-full').style.display = 'none'; document.getElementById('2102.07785v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 3 figures, 3 tables. Accepted for publication in Astronomy and Astrophysics (A&A)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 648, A70 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.06720">arXiv:2102.06720</a> <span> [<a href="https://arxiv.org/pdf/2102.06720">pdf</a>, <a href="https://arxiv.org/format/2102.06720">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab525">10.1093/mnras/stab525 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An enquiry on the origins of N-rich stars in the inner Galaxy basedon APOGEE chemical compositions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kisku%2C+S">Shobhit Kisku</a>, <a href="/search/astro-ph?searchtype=author&query=Schiavon%2C+R+P">Ricardo P. Schiavon</a>, <a href="/search/astro-ph?searchtype=author&query=Horta%2C+D">Danny Horta</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+A">Andrew Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Mackereth%2C+J+T">J. Ted Mackereth</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Hernandez%2C+D+A">D. A. Garcia-Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Bizyaev%2C+D">Dmitry Bizyaev</a>, <a href="/search/astro-ph?searchtype=author&query=Brownstein%2C+J+R">Joel R. Brownstein</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+K">Kaike Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.06720v1-abstract-short" style="display: inline;"> Recent evidence based on APOGEE data for stars within a few kpc of the Galactic centre suggests that dissolved globular clusters (GCs) contribute significantly to the stellar mass budget of the inner halo. In this paper we enquire into the origins of tracers of GC dissolution, N-rich stars, that are located in the inner 4 kpc of the Milky Way. From an analysis of the chemical compositions of these… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.06720v1-abstract-full').style.display = 'inline'; document.getElementById('2102.06720v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.06720v1-abstract-full" style="display: none;"> Recent evidence based on APOGEE data for stars within a few kpc of the Galactic centre suggests that dissolved globular clusters (GCs) contribute significantly to the stellar mass budget of the inner halo. In this paper we enquire into the origins of tracers of GC dissolution, N-rich stars, that are located in the inner 4 kpc of the Milky Way. From an analysis of the chemical compositions of these stars we establish that about 30% of the N-rich stars previously identified in the inner Galaxy may have an accreted origin. This result is confirmed by an analysis of the kinematic properties of our sample. The specific frequency of N-rich stars is quite large in the accreted population, exceeding that of its in situ counterparts by near an order of magnitude, in disagreement with predictions from numerical simulations. We hope that our numbers provide a useful test to models of GC formation and destruction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.06720v1-abstract-full').style.display = 'none'; document.getElementById('2102.06720v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages including 7 Figures and 1 Appendix. Accepted for publication by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.01706">arXiv:2102.01706</a> <span> [<a href="https://arxiv.org/pdf/2102.01706">pdf</a>, <a href="https://arxiv.org/format/2102.01706">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202040255">10.1051/0004-6361/202040255 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> APOGEE discovery of a chemically atypical star disrupted from NGC 6723 and captured by the Milky Way bulge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Carigi%2C+L">Leticia Carigi</a>, <a href="/search/astro-ph?searchtype=author&query=Placco%2C+V+M">Vinicius M. Placco</a>, <a href="/search/astro-ph?searchtype=author&query=Chun%2C+S">Sang-Hyun Chun</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">Sandro Villanova</a>, <a href="/search/astro-ph?searchtype=author&query=Souza%2C+S+O">Stefano O. Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">Angeles P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Chiappini%2C+C">Cristina Chiappini</a>, <a href="/search/astro-ph?searchtype=author&query=Queiroz%2C+A+B+A">Anna. B. A. Queiroz</a>, <a href="/search/astro-ph?searchtype=author&query=Tang%2C+B">Baitian Tang</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garc%C3%ADa%2C+J">Javier Alonso-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Piatti%2C+A+E">Andr茅s E. Piatti</a>, <a href="/search/astro-ph?searchtype=author&query=Palma%2C+T">Tali Palma</a>, <a href="/search/astro-ph?searchtype=author&query=Alves-Brito%2C+A">Alan Alves-Brito</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">Christian Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+R+R">Ricardo R. Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Singh%2C+H+P">Harinder P. Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Kundu%2C+R">Richa Kundu</a>, <a href="/search/astro-ph?searchtype=author&query=Chaves-Velasquez%2C+L">Leonardo Chaves-Velasquez</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.01706v1-abstract-short" style="display: inline;"> The central (`bulge') region of the Milky Way is teeming with a significant fraction of mildly metal-deficient stars with atmospheres that are strongly enriched in cyanogen ($^{12}$C$^{14}$N). Some of these objects, which are also known as nitrogen-enhanced stars, are hypothesised to be relics of the ancient assembly history of the Milky Way. Although the chemical similarity of nitrogen-enhanced s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.01706v1-abstract-full').style.display = 'inline'; document.getElementById('2102.01706v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.01706v1-abstract-full" style="display: none;"> The central (`bulge') region of the Milky Way is teeming with a significant fraction of mildly metal-deficient stars with atmospheres that are strongly enriched in cyanogen ($^{12}$C$^{14}$N). Some of these objects, which are also known as nitrogen-enhanced stars, are hypothesised to be relics of the ancient assembly history of the Milky Way. Although the chemical similarity of nitrogen-enhanced stars to the unique chemical patterns observed in globular clusters has been observed, a direct connection between field stars and globular clusters has not yet been proven. In this work, we report on high-resolution, near-infrared spectroscopic observations of the bulge globular cluster NGC 6723, and the serendipitous discovery of a star, 2M18594405$-$3651518, located outside the cluster (near the tidal radius) but moving on a similar orbit, providing the first clear piece of evidence of a star that was very likely once a cluster member and has recently been ejected. Its nitrogen abundance ratio ([N/Fe]$\gtrsim + 0.94$) is well above the typical Galactic field-star levels, and it exhibits noticeable enrichment in the heavy $s$-process elements (Ce, Nd, and Yb), along with moderate carbon enrichment; all characteristics are known examples in globular clusters. This result suggests that some of the nitrogen-enhanced stars in the bulge likely originated from the tidal disruption of globular clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.01706v1-abstract-full').style.display = 'none'; document.getElementById('2102.01706v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Astronomy & Astrophysics, in press. 16 pages, 8 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.01088">arXiv:2102.01088</a> <span> [<a href="https://arxiv.org/pdf/2102.01088">pdf</a>, <a href="https://arxiv.org/format/2102.01088">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/abdf47">10.3847/2041-8213/abdf47 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VVV CL001: Likely the Most Metal-Poor Surviving Globular Cluster in the Inner Galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Souza%2C+S+O">Stefano O. Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">Christian Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">Sandro Villanova</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">Angeles P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Henao%2C+L">Lady Henao</a>, <a href="/search/astro-ph?searchtype=author&query=Romero-Colmenares%2C+M">Mar铆a Romero-Colmenares</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.01088v2-abstract-short" style="display: inline;"> We present the first high-resolution abundance analysis of the globular cluster VVV~CL001, which resides in a region dominated by high interstellar reddening towards the Galactic Bulge. Using \textit{H}-band spectra acquired by the Apache Point Observatory Galactic Evolution Experiment (APOGEE), we identified two potential members of the cluster, and estimate from their Fe I lines that the cluster… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.01088v2-abstract-full').style.display = 'inline'; document.getElementById('2102.01088v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.01088v2-abstract-full" style="display: none;"> We present the first high-resolution abundance analysis of the globular cluster VVV~CL001, which resides in a region dominated by high interstellar reddening towards the Galactic Bulge. Using \textit{H}-band spectra acquired by the Apache Point Observatory Galactic Evolution Experiment (APOGEE), we identified two potential members of the cluster, and estimate from their Fe I lines that the cluster has an average metallicity of [Fe/H] = $-2.45$ with an uncertainty due to systematics of 0.24 dex. We find that the light-(N), $伪$-(O, Mg, Si), and Odd-Z (Al) elemental abundances of the stars in VVV~CL001 follow the same trend as other Galactic metal-poor globular clusters. This makes VVV~CL001 possibly the most metal-poor globular cluster identified so far within the Sun's galactocentric distance and likely one of the most metal-deficient clusters in the Galaxy after ESO280-SC06. Applying statistical isochrone fitting, we derive self-consistent age, distance, and reddening values, yielding an estimated age of $11.9^{+3.12}_{-4.05}$ Gyr at a distance of $8.22^{+1.84}_{-1.93}$ kpc, revealing that VVV~CL001 is also an old GC in the inner Galaxy. The Galactic orbit of VVV~CL001 indicates that this cluster lies on a halo-like orbit that appears to be highly eccentric. Both chemistry and dynamics support the hypothesis that VVV~CL001 could be an ancient fossil relic left behind by a massive merger event during the early evolution of the Galaxy, likely associated with either the Sequoia or the \textit{Gaia}-Enceladus-Sausage structures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.01088v2-abstract-full').style.display = 'none'; document.getElementById('2102.01088v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal Letters. 9 pages, 4 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.04488">arXiv:2101.04488</a> <span> [<a href="https://arxiv.org/pdf/2101.04488">pdf</a>, <a href="https://arxiv.org/format/2101.04488">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab2899">10.1093/mnras/stab2899 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The distribution of [$伪$/Fe] in the Milky Way disc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vincenzo%2C+F">Fiorenzo Vincenzo</a>, <a href="/search/astro-ph?searchtype=author&query=Weinberg%2C+D+H">David H. Weinberg</a>, <a href="/search/astro-ph?searchtype=author&query=Miglio%2C+A">Andrea Miglio</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.04488v2-abstract-short" style="display: inline;"> Using a sample of red giant stars from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) Data Release 16, we infer the conditional distribution $p([伪/\text{Fe}]\,|\,[\text{Fe/H}])$ in the Milky Way disk for the $伪$-elements Mg, O, Si, S, and Ca. In each bin of [Fe/H] and Galactocentric radius $R$, we model $p([伪/\text{Fe}])$ as a sum of two Gaussians, representing "low-$伪$" and "… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.04488v2-abstract-full').style.display = 'inline'; document.getElementById('2101.04488v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.04488v2-abstract-full" style="display: none;"> Using a sample of red giant stars from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) Data Release 16, we infer the conditional distribution $p([伪/\text{Fe}]\,|\,[\text{Fe/H}])$ in the Milky Way disk for the $伪$-elements Mg, O, Si, S, and Ca. In each bin of [Fe/H] and Galactocentric radius $R$, we model $p([伪/\text{Fe}])$ as a sum of two Gaussians, representing "low-$伪$" and "high-$伪$" populations with scale heights $z_1=0.45\,\text{kpc}$ and $z_2=0.95\,\text{kpc}$, respectively. By accounting for age-dependent and $z$-dependent selection effects in APOGEE, we infer the [$伪$/Fe] distributions that would be found for a fair sample of long-lived stars covering all $z$. Near the Solar circle, this distribution is bimodal at sub-solar [Fe/H], with the low-$伪$ and high-$伪$ peaks clearly separated by a minimum at intermediate [$伪$/Fe]. In agreement with previous results, we find that the high-$伪$ population is more prominent at smaller $R$, lower [Fe/H], and larger $|z|$, and that the sequence separation is smaller for Si and Ca than for Mg, O, and S. We find significant intrinsic scatter in [$伪$/Fe] at fixed [Fe/H] for both the low-$伪$ and high-$伪$ populations, typically $\sim 0.04$-dex. The means, dispersions, and relative amplitudes of this two-Gaussian description, and the dependence of these parameters on $R$, [Fe/H], and $伪$-element, provide a quantitative target for chemical evolution models and a test for hydrodynamic simulations of disk galaxy formation. We argue that explaining the observed bimodality will probably require one or more sharp transitions in the disk's gas accretion, star formation, or outflow history in addition to radial mixing of stellar populations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.04488v2-abstract-full').style.display = 'none'; document.getElementById('2101.04488v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.15773">arXiv:2012.15773</a> <span> [<a href="https://arxiv.org/pdf/2012.15773">pdf</a>, <a href="https://arxiv.org/format/2012.15773">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/abd7f1">10.3847/1538-3881/abd7f1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The APOGEE Library of Infrared SSP Templates (A-LIST): High-Resolution Simple Stellar Population Spectral Models in the H-Band </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ashok%2C+A">Aishwarya Ashok</a>, <a href="/search/astro-ph?searchtype=author&query=Zasowski%2C+G">Gail Zasowski</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A">Anil Seth</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Bergsten%2C+G">Galen Bergsten</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+O">Olivia Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Boardman%2C+N">Nicholas Boardman</a>, <a href="/search/astro-ph?searchtype=author&query=Bizyaev%2C+D">Dmitry Bizyaev</a>, <a href="/search/astro-ph?searchtype=author&query=Goytia%2C+S+M">Sofia Meneses Goytia</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Hern%C3%A1ndez%2C+D+A">D. A. Garc铆a-Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.15773v1-abstract-short" style="display: inline;"> Integrated light spectroscopy from galaxies can be used to study the stellar populations that cannot be resolved into individual stars. This analysis relies on stellar population synthesis (SPS) techniques to study the formation history and structure of galaxies. However, the spectral templates available for SPS are limited, especially in the near-infrared. We present A-LIST (APOGEE Library of Inf… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.15773v1-abstract-full').style.display = 'inline'; document.getElementById('2012.15773v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.15773v1-abstract-full" style="display: none;"> Integrated light spectroscopy from galaxies can be used to study the stellar populations that cannot be resolved into individual stars. This analysis relies on stellar population synthesis (SPS) techniques to study the formation history and structure of galaxies. However, the spectral templates available for SPS are limited, especially in the near-infrared. We present A-LIST (APOGEE Library of Infrared SSP Templates), a new set of high-resolution, near-IR SSP spectral templates spanning a wide range of ages (2-12 Gyr), metallicities ($\rm -2.2 < [M/H] < +0.4$) and $伪$ abundances ($\rm -0.2 < [伪/M] < +0.4$). This set of SSP templates is the highest resolution ($R\sim22500$) available in the near infrared, and the first such based on an empirical stellar library. Our models are generated using spectra of $\sim$300,000 stars spread across the Milky Way, with a wide range of metallicities and abundances, from the APOGEE survey. We show that our model spectra provide accurate fits to M31 globular cluster spectra taken with APOGEE, with best-fit metallicities agreeing with those of previous estimates to within $\sim$0.1 dex. We also compare these model spectra to lower-resolution E-MILES models and demonstrate that we recover the ages of these models to within $\sim$1.5 Gyr. This library is available in https://github.com/aishashok/ALIST-library. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.15773v1-abstract-full').style.display = 'none'; document.getElementById('2012.15773v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 15 figures, accepted for publication in The Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.12997">arXiv:2012.12997</a> <span> [<a href="https://arxiv.org/pdf/2012.12997">pdf</a>, <a href="https://arxiv.org/format/2012.12997">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/abd62e">10.3847/1538-3881/abd62e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Analysis of Previously Classified White Dwarf-Main Sequence Binaries Using Data from the APOGEE Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Corcoran%2C+K+A">Kyle A. Corcoran</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+H+M">Hannah M. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Anguiano%2C+B">Borja Anguiano</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Kounkel%2C+M">Marina Kounkel</a>, <a href="/search/astro-ph?searchtype=author&query=McDonald%2C+D+J">Devin J McDonald</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+V">Verne Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Badenes%2C+C">Carles Badenes</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lee%2C+N">Nathan De Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzola%2C+C+N">Christine N. Mazzola</a>, <a href="/search/astro-ph?searchtype=author&query=Longa-Pe%C3%B1a%2C+P">Pen茅lope Longa-Pe帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.12997v1-abstract-short" style="display: inline;"> We present analyses of near-infrared, spectroscopic data from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey for 45 previously confirmed or candidate white dwarf-main sequence (WDMS) binaries identified by the optical SDSS and LAMOST surveys. Among these 45 systems, we classify three as having red giant primaries in the LAMOST sample and fourteen to be young stellar obj… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12997v1-abstract-full').style.display = 'inline'; document.getElementById('2012.12997v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.12997v1-abstract-full" style="display: none;"> We present analyses of near-infrared, spectroscopic data from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey for 45 previously confirmed or candidate white dwarf-main sequence (WDMS) binaries identified by the optical SDSS and LAMOST surveys. Among these 45 systems, we classify three as having red giant primaries in the LAMOST sample and fourteen to be young stellar object contaminants in the photometrically identified SDSS sample. From among the subsample of 28 systems that we confirm to have MS primaries, we derive and place limits on orbital periods and velocity amplitudes for fourteen. Seven systems have significant velocity variations that warrant a post-common-envelope (PCE) binary classification -- four of which are newly classified, three of which are newly confirmed, and five for which we can derive full orbital parameters. If confirmed, one of these newly discovered systems (2M14544500+4626456) will have the second longest orbital period reported for a typical, compact PCE WDMS binary ($P=15.1$ days). In addition to the seven above, we also recover and characterize with APOGEE data the well known PCE WDMS systems EG UMa and HZ 9. We also investigate the overall metallicity distribution of the WDMS sample, which is a parameter space not often explored for these systems. Of note, we find one system (2M14244053+4929580) to be extremely metal-poor (${\rm [Fe/H]}=-1.42$) relative to the rest of the near-solar sample. Additionally, the PCE systems in our sample are found to be, on average, higher in metallicity than their wide-binary counterparts, though we caution that with this small number of systems, the sample may not be representative of the overall distribution of WDMS systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12997v1-abstract-full').style.display = 'none'; document.getElementById('2012.12997v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 10 figures, accepted for publication by AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.10398">arXiv:2010.10398</a> <span> [<a href="https://arxiv.org/pdf/2010.10398">pdf</a>, <a href="https://arxiv.org/format/2010.10398">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abc3c2">10.3847/1538-4357/abc3c2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the Galactic Warp Through Asymmetries in the Kinematics of the Galactic Disk </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+X">Xinlun Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Anguiano%2C+B">Borja Anguiano</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Hayes%2C+C">Christian Hayes</a>, <a href="/search/astro-ph?searchtype=author&query=Arras%2C+P">Phil Arras</a>, <a href="/search/astro-ph?searchtype=author&query=Chiappini%2C+C">Cristina Chiappini</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Queiroz%2C+A+B+d+A">Anna B谩rbara de Andrade Queiroz</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C4%B1a-Hern%C3%A1ndez%2C+D+A">Domingo An谋bal Garc谋a-Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P">Peter Frinchaboy</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.10398v1-abstract-short" style="display: inline;"> Previous analyses of large databases of Milky Way stars have revealed the stellar disk of our Galaxy to be warped and that this imparts a strong signature on the kinematics of stars beyond the solar neighborhood. However, due to the limitation of accurate distance estimates, many attempts to explore the extent of these Galactic features have generally been restricted to a volume near the Sun. By c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.10398v1-abstract-full').style.display = 'inline'; document.getElementById('2010.10398v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.10398v1-abstract-full" style="display: none;"> Previous analyses of large databases of Milky Way stars have revealed the stellar disk of our Galaxy to be warped and that this imparts a strong signature on the kinematics of stars beyond the solar neighborhood. However, due to the limitation of accurate distance estimates, many attempts to explore the extent of these Galactic features have generally been restricted to a volume near the Sun. By combining Gaia DR2 astrometric solution, StarHorse distance and stellar abundances from the APOGEE survey, we present the most detailed and radially expansive study yet of the vertical and radial motions of stars in the Galactic disk. We map stellar velocity with respect to their Galactocentric radius, angular momentum, and azimuthal angle and assess their relation to the warp. A decrease in vertical velocity is discovered at Galactocentric radius $R=13\ \text{kpc}$ and angular momentum $L_z=2800\ \text{kpc}\ \text{km}\ \text{s}^{-1}$. Smaller ripples in vertical and radial velocity are also discovered superposed on the main trend. We also discovered that trends in the vertical velocity with azimuthal angle are not symmetric about the peak, suggesting the warp to be lopsided. To explain the global trend in vertical velocity, we built a simple analytical model of the Galactic warp. Our best fit yields a starting radius of $8.87^{+0.08}_{-0.09}\ \text{kpc}$ and precession rate of $13.57^{+0.20}_{-0.18}\ \text{km}\ \text{s}^{-1}\ \text{kpc}^{-1}$. These parameters remain consistent across stellar age groups, a result that supports the notion that the warp is the result of an external, gravitationally induced phenomenon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.10398v1-abstract-full').style.display = 'none'; document.getElementById('2010.10398v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.00024">arXiv:2010.00024</a> <span> [<a href="https://arxiv.org/pdf/2010.00024">pdf</a>, <a href="https://arxiv.org/format/2010.00024">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/abc01d">10.3847/2041-8213/abc01d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a large population of Nitrogen-Enhanced stars in the Magellanic Clouds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Carigi%2C+L">Leticia Carigi</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Placco%2C+V+M">Vinicius M. Placco</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">Christian Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">Sandro Villanova</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.00024v1-abstract-short" style="display: inline;"> We report the APOGEE-2S$+$ discovery of a unique collection of nitrogen-enhanced mildly metal-poor giant stars, peaking at [Fe/H]$\sim -0.89$ with no carbon enrichment, toward the Small and Large Magellanic Clouds (MCs), with abundances of light- (C, N), odd-Z (Al, K) and $伪-$elements (O, Mg, Si) that are typically found in Galactic globular clusters (GCs). Here we present 44 stars in the MCs that… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.00024v1-abstract-full').style.display = 'inline'; document.getElementById('2010.00024v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.00024v1-abstract-full" style="display: none;"> We report the APOGEE-2S$+$ discovery of a unique collection of nitrogen-enhanced mildly metal-poor giant stars, peaking at [Fe/H]$\sim -0.89$ with no carbon enrichment, toward the Small and Large Magellanic Clouds (MCs), with abundances of light- (C, N), odd-Z (Al, K) and $伪-$elements (O, Mg, Si) that are typically found in Galactic globular clusters (GCs). Here we present 44 stars in the MCs that exhibit significantly enhanced [N/Fe] abundance ratios, well above ([N/Fe]$>+0.6$) typical Galactic levels at similar metallicity, and a star that is very nitrogen-enhanced ([N/Fe]$> +2.45$). Our sample consists of luminous evolved stars on the asymptotic giant branch (AGB), eight of which are classified as bonafide semi-regular (SR) variables, as well as low-luminosity stars similar to that of stars on the tip of the red giant branch of stellar clusters in the MCs. It seems likely that whatever nucleosynthetic process is responsible for these anomalous MC stars it is similar to that which caused the common stellar populations in GCs. We interpret these distinctive C-N patterns as the observational evidence of the result of tidally shredded GCs in the MCs. These findings might explain some previous conflicting results over bulge N-rich stars, and broadly help to understand GC formation and evolution. Furthermore, the discovery of such a large population of N-rich AGB stars in the MCs suggests that multiple stellar populations might not only be exotic events from the past but can also form at lower redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.00024v1-abstract-full').style.display = 'none'; document.getElementById('2010.00024v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ Letters; 11 pages, 4 Figures, 1 Table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.05063">arXiv:2009.05063</a> <span> [<a href="https://arxiv.org/pdf/2009.05063">pdf</a>, <a href="https://arxiv.org/format/2009.05063">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abd6be">10.3847/1538-4357/abd6be <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Similarity of Abundance Ratio Trends and Nucleosynthetic Patterns in the Milky Way Disk and Bulge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Griffith%2C+E">Emily Griffith</a>, <a href="/search/astro-ph?searchtype=author&query=Weinberg%2C+D+H">David H. Weinberg</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J+A">Jennifer A. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachael Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Hern%C3%A1ndez%2C+D+A">D. A. Garc铆a-Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Holtzman%2C+J">Jon Holtzman</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J+W">James W. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B6nsson%2C+H">Henrik J枚nsson</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Nataf%2C+D+M">David M. Nataf</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.05063v2-abstract-short" style="display: inline;"> We compare abundance ratio trends in a sample of $\sim 11,000$ Milky Way bulge stars ($R_{\rm GC} < 3$ kpc) from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) to those of APOGEE stars in the Galactic disk ($5$ kpc $< R_{\rm GC} < 11$ kpc). We divide each sample into low-Ia (high-[Mg/Fe]) and high-Ia (low-[Mg/Fe]) populations, and in each population we examine the median trend… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.05063v2-abstract-full').style.display = 'inline'; document.getElementById('2009.05063v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.05063v2-abstract-full" style="display: none;"> We compare abundance ratio trends in a sample of $\sim 11,000$ Milky Way bulge stars ($R_{\rm GC} < 3$ kpc) from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) to those of APOGEE stars in the Galactic disk ($5$ kpc $< R_{\rm GC} < 11$ kpc). We divide each sample into low-Ia (high-[Mg/Fe]) and high-Ia (low-[Mg/Fe]) populations, and in each population we examine the median trends of [X/Mg] vs. [Mg/H] for elements X = Fe, O, Na, Al, Si, P, S, K, Ca, V, Cr, Mn, Co, Ni, Cu, and Ce. To remove small systematic trends of APOGEE abundances with stellar $\log(g)$, we resample the disk stars to match the $\log(g)$ distributions of the bulge data. After doing so, we find nearly identical median trends for low-Ia disk and bulge stars for all elements. High-Ia trends are similar for most elements, with noticeable (0.05-0.1 dex) differences for Mn, Na, and Co. The close agreement of abundance trends (with typical differences $\lesssim 0.03$ dex) implies that similar nucleosynthetic processes enriched bulge and disk stars despite the different star formation histories and physical conditions of these regions. For example, we infer that differences in the high mass slope of the stellar initial mass function (IMF) between disk and bulge must have been $\lesssim 0.30$. This agreement, and the generally small scatter about the median sequences, means that one can predict all of a bulge star's APOGEE abundances with good accuracy knowing only its measured [Mg/Fe] and [Mg/H] and the observed trends of disk stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.05063v2-abstract-full').style.display = 'none'; document.getElementById('2009.05063v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 22 figures, 5 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.04399">arXiv:2008.04399</a> <span> [<a href="https://arxiv.org/pdf/2008.04399">pdf</a>, <a href="https://arxiv.org/ps/2008.04399">ps</a>, <a href="https://arxiv.org/format/2008.04399">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa2425">10.1093/mnras/staa2425 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VISCACHA survey -- II. Structure of star clusters in the Magellanic Clouds periphery </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J+F+C">J. F. C. Santos Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F+F+S">F. F. S. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L+d+O">L. de O. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Piatti%2C+A+E">A. E. Piatti</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Angelo%2C+M+S">M. S. Angelo</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">A. P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">A. Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Westera%2C+P">P. Westera</a>, <a href="/search/astro-ph?searchtype=author&query=Fraga%2C+L">L. Fraga</a>, <a href="/search/astro-ph?searchtype=author&query=Quint%2C+B">B. Quint</a>, <a href="/search/astro-ph?searchtype=author&query=Sanmartim%2C+D">D. Sanmartim</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2008.04399v1-abstract-short" style="display: inline;"> We provide a homogeneous set of structural parameters of 83 star clusters located at the periphery of the Small Magellanic Cloud (SMC) and the Large Magellanic Cloud (LMC). The clusters' stellar density and surface brightness profiles were built from deep, AO assisted optical images, and uniform analysis techniques. The structural parameters were obtained from King and Elson et al. model fittings.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.04399v1-abstract-full').style.display = 'inline'; document.getElementById('2008.04399v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.04399v1-abstract-full" style="display: none;"> We provide a homogeneous set of structural parameters of 83 star clusters located at the periphery of the Small Magellanic Cloud (SMC) and the Large Magellanic Cloud (LMC). The clusters' stellar density and surface brightness profiles were built from deep, AO assisted optical images, and uniform analysis techniques. The structural parameters were obtained from King and Elson et al. model fittings. Integrated magnitudes and masses (for a subsample) are also provided. The sample contains mostly low surface brightness clusters with distances between 4.5 and 6.5 kpc and between 1 and 6.5 kpc from the LMC and SMC centres, respectively. We analysed their spatial distribution and structural properties, comparing them with those of inner clusters. Half-light and Jacobi radii were estimated, allowing an evaluation of the Roche volume tidal filling. We found that: (i) for our sample of LMC clusters, the tidal radii are, on average, larger than those of inner clusters from previous studies; (ii) the core radii dispersion tends to be greater for LMC clusters located towards the southwest, with position angles of $\sim$200 degrees and about $\sim$5 degrees from the LMC centre, i.e., those LMC clusters nearer to the SMC; (iii) the core radius evolution for clusters with known age is similar to that of inner clusters; (iv) SMC clusters with galactocentric distances closer than 4 kpc are overfilling; (v) the recent Clouds collision did not leave marks on the LMC clusters' structure that our analysis could reveal. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.04399v1-abstract-full').style.display = 'none'; document.getElementById('2008.04399v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 16 figures, accepted by MNRAS. Full tables and additional plots included</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.03603">arXiv:2008.03603</a> <span> [<a href="https://arxiv.org/pdf/2008.03603">pdf</a>, <a href="https://arxiv.org/format/2008.03603">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abaeee">10.3847/1538-4357/abaeee <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the stellar age distribution of the Milky Way Bulge using APOGEE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Zasowski%2C+G">Gail Zasowski</a>, <a href="/search/astro-ph?searchtype=author&query=Feuillet%2C+D+K">Diane K. Feuillet</a>, <a href="/search/astro-ph?searchtype=author&query=Schultheis%2C+M">Mathias Schultheis</a>, <a href="/search/astro-ph?searchtype=author&query=Nataf%2C+D+M">David M. Nataf</a>, <a href="/search/astro-ph?searchtype=author&query=Anguiano%2C+B">Borja Anguiano</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Hern%C3%A1ndez%2C+D+A">D. A. Garc铆a-Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Holtzman%2C+J+A">Jon A. Holtzman</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J">Jennifer Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">Christian Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Schiavon%2C+R">Ricardo Schiavon</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+V+V">Verne V. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sobeck%2C+J">Jennifer Sobeck</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2008.03603v1-abstract-short" style="display: inline;"> We present stellar age distributions of the Milky Way (MW) bulge region using ages for $\sim$6,000 high-luminosity ($\log(g) < 2.0$), metal-rich ($\rm [Fe/H] \ge -0.5$) bulge stars observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE). Ages are derived using {\it The Cannon} label-transfer method, trained on a sample of nearby luminous giants with precise parallaxes for w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.03603v1-abstract-full').style.display = 'inline'; document.getElementById('2008.03603v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.03603v1-abstract-full" style="display: none;"> We present stellar age distributions of the Milky Way (MW) bulge region using ages for $\sim$6,000 high-luminosity ($\log(g) < 2.0$), metal-rich ($\rm [Fe/H] \ge -0.5$) bulge stars observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE). Ages are derived using {\it The Cannon} label-transfer method, trained on a sample of nearby luminous giants with precise parallaxes for which we obtain ages using a Bayesian isochrone-matching technique. We find that the metal-rich bulge is predominantly composed of old stars ($>$8 Gyr). We find evidence that the planar region of the bulge ($|Z_{\rm GC}| \le 0.25$ kpc) enriched in metallicity, $Z$, at a faster rate ($dZ/dt \sim$ 0.0034 ${\rm Gyr^{-1}}$) than regions farther from the plane ($dZ/dt \sim$ 0.0013 ${\rm Gyr^{-1}}$ at $|Z_{\rm GC}| > 1.00$ kpc). We identify a non-negligible fraction of younger stars (age $\sim$ 2--5 Gyr) at metallicities of $\rm +0.2 < [Fe/H] < +0.4$. These stars are preferentially found in the plane ($|Z_{\rm GC}| \le 0.25$ kpc) and between $R_{\rm cy} \approx 2-3$ kpc, with kinematics that are more consistent with rotation than are the kinematics of older stars at the same metallicities. We do not measure a significant age difference between stars found in and outside of the bar. These findings show that the bulge experienced an initial starburst that was more intense close to the plane than far from the plane. Then, star formation continued at super-solar metallicities in a thin disk at 2 kpc $\lesssim R_{\rm cy} \lesssim$ 3 kpc until $\sim$2 Gyr ago. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.03603v1-abstract-full').style.display = 'none'; document.getElementById('2008.03603v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 15 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.03320">arXiv:2008.03320</a> <span> [<a href="https://arxiv.org/pdf/2008.03320">pdf</a>, <a href="https://arxiv.org/format/2008.03320">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa3256">10.1093/mnras/staa3256 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The chemical properties of the Milky Way's on-bar and off-bar regions: evidence for inhomogeneous star formation history in the bulge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lian%2C+J">Jianhui Lian</a>, <a href="/search/astro-ph?searchtype=author&query=Zasowski%2C+G">Gail Zasowski</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+J">Justus Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Longa-Pe%C3%B1a%2C+P">Pen茅lope Longa-Pe帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2008.03320v2-abstract-short" style="display: inline;"> Numerous studies of integrated starlight, stellar counts, and kinematics have confirmed that the Milky Way is a barred galaxy. However, far fewer studies have investigated the bar's stellar population properties, which carry valuable independent information regarding the bar's formation history. Here we conduct a detailed analysis of chemical abundance distributions ([Fe/H] and [Mg/Fe]) in the on-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.03320v2-abstract-full').style.display = 'inline'; document.getElementById('2008.03320v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.03320v2-abstract-full" style="display: none;"> Numerous studies of integrated starlight, stellar counts, and kinematics have confirmed that the Milky Way is a barred galaxy. However, far fewer studies have investigated the bar's stellar population properties, which carry valuable independent information regarding the bar's formation history. Here we conduct a detailed analysis of chemical abundance distributions ([Fe/H] and [Mg/Fe]) in the on-bar and off-bar regions to study the azimuthal variation of star formation history (SFH) in the inner Galaxy. We find that the on-bar and off-bar stars at Galactocentric radii 3 $< r_{\rm GC}<$ 5 kpc have remarkably consistent [Fe/H] and [Mg/Fe] distribution functions and [Mg/Fe]--[Fe/H] relation, suggesting a common SFH shared by the long bar and the disc. In contrast, the bar and disc at smaller radii (2 $< r_{\rm GC} <$ 3 kpc) show noticeable differences, with relatively more very metal-rich ([Fe/H]~0.4) stars but fewer solar abundance stars in the bar. Given the three-phase star formation history proposed for the inner Galaxy in Lian et al. (2020b), these differences could be explained by the off-bar disc having experienced either a faster early quenching process or recent metal-poor gas accretion. Vertical variations of the abundance distributions at small $r_{\rm GC}$ suggest a wider vertical distribution of low-$伪$ stars in the bar, which may serve as chemical evidence for vertical heating through the bar buckling process. The lack of such vertical variations outside the bulge may then suggest a lack of vertical heating in the long bar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.03320v2-abstract-full').style.display = 'none'; document.getElementById('2008.03320v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 5 figures. MNRAS in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.01097">arXiv:2008.01097</a> <span> [<a href="https://arxiv.org/pdf/2008.01097">pdf</a>, <a href="https://arxiv.org/format/2008.01097">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa3598">10.1093/mnras/staa3598 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The contribution of N-rich stars to the Galactic stellar halo using APOGEE red giants </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Horta%2C+D">Danny Horta</a>, <a href="/search/astro-ph?searchtype=author&query=Mackereth%2C+J+T">J. Ted Mackereth</a>, <a href="/search/astro-ph?searchtype=author&query=Schiavon%2C+R+P">Ricardo P. Schiavon</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Bovy%2C+J">Jo Bovy</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Hern%C3%A1ndez%2C+D+A">D. A. Garc铆a-Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Kisku%2C+S+S">Shobhit S. Kisku</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+A+C">Andrew C. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Nataf%2C+D+M">David M. Nataf</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Schultheis%2C+M">Mathias Schultheis</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2008.01097v3-abstract-short" style="display: inline;"> The contribution of dissolved globular clusters (GCs) to the stellar content of the Galactic halo is a key constraint on models for GC formation and destruction, and the mass assembly history of the Milky Way. Earlier results from APOGEE pointed to a large contribution of destroyed GCs to the stellar content of the inner halo, by as much as 25$\%$, which is an order of magnitude larger than previo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.01097v3-abstract-full').style.display = 'inline'; document.getElementById('2008.01097v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.01097v3-abstract-full" style="display: none;"> The contribution of dissolved globular clusters (GCs) to the stellar content of the Galactic halo is a key constraint on models for GC formation and destruction, and the mass assembly history of the Milky Way. Earlier results from APOGEE pointed to a large contribution of destroyed GCs to the stellar content of the inner halo, by as much as 25$\%$, which is an order of magnitude larger than previous estimates for more distant regions of the halo. We set out to measure the ratio between N-rich and normal halo field stars, as a function of distance, by performing density modelling of halo field populations in APOGEE DR16. Our results show that at 1.5 kpc from the Galactic Centre, N-rich stars contribute a much higher 16.8$^{+10.0}_{-7.0}$$\%$ fraction to the total stellar halo mass budget than the 2.7$^{+1.0}_{-0.8}$$\%$ ratio contributed at 10 kpc. Under the assumption that N-rich stars are former GC members that now reside in the stellar halo field, and assuming the ratio between first-and second-population GC stars being 1:2, we estimate a total contribution from disrupted GC stars of the order of 27.5$^{+15.4}_{-11.5}$$\%$ at r = 1.5 kpc and 4.2$^{+1.5}_{-1.3}$$\%$ at r = 10 kpc. Furthermore, since our methodology requires fitting a density model to the stellar halo, we integrate such density within a spherical shell from 1.5-15 kpc in radius, and find a total stellar mass arising from dissolved and/or evaporated GCs of $M_{\mathrm{GC,total}}$ = 9.6$^{+4.0}_{-2.6}$ $\times$ 10$^{7}$ M$\odot$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.01097v3-abstract-full').style.display = 'none'; document.getElementById('2008.01097v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Paper accepted for Publication in MNRAS, correction of Fig 7</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.12915">arXiv:2007.12915</a> <span> [<a href="https://arxiv.org/pdf/2007.12915">pdf</a>, <a href="https://arxiv.org/format/2007.12915">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202039030">10.1051/0004-6361/202039030 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Milky Way bar and bulge revealed by APOGEE DR16 and Gaia EDR3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Queiroz%2C+A+B+A">A. B. A. Queiroz</a>, <a href="/search/astro-ph?searchtype=author&query=Chiappini%2C+C">C. Chiappini</a>, <a href="/search/astro-ph?searchtype=author&query=Perez-Villegas%2C+A">A. Perez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Khalatyan%2C+A">A. Khalatyan</a>, <a href="/search/astro-ph?searchtype=author&query=Anders%2C+F">F. Anders</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Santiago%2C+B+X">B. X. Santiago</a>, <a href="/search/astro-ph?searchtype=author&query=Steinmetz%2C+M">M. Steinmetz</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">K. Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Schultheis%2C+M">M. Schultheis</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">S. R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Minchev%2C+I">I. Minchev</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">R. L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">R. E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=da+Costa%2C+L+N">L. N. da Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">J. G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Hern%C3%A1ndez%2C+D+A">D. A. Garcia-Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">S. Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">R. R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">C. Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+A">A. Rojas-Arriagada</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">A. Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+V">V. Smith</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.12915v4-abstract-short" style="display: inline;"> We investigate the inner regions of the Milky Way with a sample of unprecedented size and coverage thanks to APOGEE DR16 and Gaia EDR3 data. Our inner Galactic sample has more than 26,000 stars within $|X_{\rm Gal}| <5$ kpc, $|Y_{\rm Gal}| <3.5$ kpc, $|Z_{\rm Gal}| <1$ kpc, and we also make the analysis for a foreground-cleaned sub-sample of 8,000 stars more representative of the bulge-bar populat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.12915v4-abstract-full').style.display = 'inline'; document.getElementById('2007.12915v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.12915v4-abstract-full" style="display: none;"> We investigate the inner regions of the Milky Way with a sample of unprecedented size and coverage thanks to APOGEE DR16 and Gaia EDR3 data. Our inner Galactic sample has more than 26,000 stars within $|X_{\rm Gal}| <5$ kpc, $|Y_{\rm Gal}| <3.5$ kpc, $|Z_{\rm Gal}| <1$ kpc, and we also make the analysis for a foreground-cleaned sub-sample of 8,000 stars more representative of the bulge-bar populations. The inner Galaxy shows a clear chemical discontinuity in key abundance ratios [$伪$/Fe], [C/N], and [Mn/O], probing different enrichment timescales, which suggests a star formation gap (quenching) between the high- and low-$伪$ populations. For the first time, we are able to fully characterize the different populations co-existing in the innermost regions of the Galaxy via joint analysis of the distributions of rotational velocities, metallicities, orbital parameters and chemical abundances. The chemo-kinematic analysis reveals the presence of the bar; of an inner thin disk; of a thick disk, and of a broad metallicity population, with a large velocity dispersion, indicative of a pressure supported component. We find and characterize chemically and kinematically a group of counter-rotating stars, which could be the result of a gas-rich merger event or just the result of clumpy star formation during the earliest phases of the early disk, which migrated into the bulge. Finally, based on the 6D information we assign stars a probability value of being on a bar orbit and find that most of the stars with large bar orbit probabilities come from the innermost 3 kpcs. Even stars with a high probability of belonging to the bar show the chemical bimodality in the [$伪$/Fe] vs. [Fe/H] diagram. This suggests bar trapping to be an efficient mechanism, explaining why stars on bar orbits do not show a significant distinct chemical abundance ratio signature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.12915v4-abstract-full').style.display = 'none'; document.getElementById('2007.12915v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 25 figures, Accepted for publication on A&A, in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 656, A156 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.12179">arXiv:2007.12179</a> <span> [<a href="https://arxiv.org/pdf/2007.12179">pdf</a>, <a href="https://arxiv.org/format/2007.12179">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa2205">10.1093/mnras/staa2205 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Milky Way's bulge star formation history as constrained from its bimodal chemical abundance distribution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lian%2C+J">Jianhui Lian</a>, <a href="/search/astro-ph?searchtype=author&query=Zasowski%2C+G">Gail Zasowski</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Nataf%2C+D+M">David M. Nataf</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+D">Daniel Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">Christian Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Hernandez%2C+D+A">D. A. Garcia-Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Schultheis%2C+M">Mathias Schultheis</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.12179v1-abstract-short" style="display: inline;"> We conduct a quantitative analysis of the star formation history (SFH) of the Milky Way's bulge by exploiting the constraining power of its stellar [Fe/H] and [Mg/Fe] distribution functions. Using APOGEE data, we confirm the previously-established bimodal [Mg/Fe]--[Fe/H] distribution within 3 kpc of the inner Galaxy. Compared to that in the solar vicinity, the high-$伪$ population in the bulge peak… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.12179v1-abstract-full').style.display = 'inline'; document.getElementById('2007.12179v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.12179v1-abstract-full" style="display: none;"> We conduct a quantitative analysis of the star formation history (SFH) of the Milky Way's bulge by exploiting the constraining power of its stellar [Fe/H] and [Mg/Fe] distribution functions. Using APOGEE data, we confirm the previously-established bimodal [Mg/Fe]--[Fe/H] distribution within 3 kpc of the inner Galaxy. Compared to that in the solar vicinity, the high-$伪$ population in the bulge peaks at a lower [Fe/H]. To fit these observations, we use a simple but flexible star formation framework, which assumes two distinct stages of gas accretion and star formation, and systematically evaluate a wide multi-dimensional parameter space. We find that the data favor a three-phase SFH that consists of an initial starburst, followed by a rapid star formation quenching episode and a lengthy, quiescent secular evolution phase. The metal-poor, high-$伪$ bulge stars ([Fe/H]<0.0 and [Mg/Fe]>0.15) are formed rapidly (<2 Gyr) during the early starburst. The density gap between the high- and low-$伪$ sequences is due to the quenching process. The metal-rich, low-$伪$ population ([Fe/H]>0.0 and [Mg/Fe]<0.15) then accumulates gradually through inefficient star formation during the secular phase. This is qualitatively consistent with the early SFH of the inner disk. Given this scenario, a notable fraction of young stars (age<5 Gyr) is expected to persist in the bulge. Combined with extragalactic observations, these results suggest that a rapid star formation quenching process is responsible for bimodal distributions in both the Milky Way's stellar populations and in the general galaxy population and thus plays a critical role in galaxy evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.12179v1-abstract-full').style.display = 'none'; document.getElementById('2007.12179v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 12 figures. MNRAS in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.09059">arXiv:2007.09059</a> <span> [<a href="https://arxiv.org/pdf/2007.09059">pdf</a>, <a href="https://arxiv.org/format/2007.09059">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa2859">10.1093/mnras/staa2859 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Close Binary Fraction as a Function of Stellar Parameters in APOGEE: A Strong Anti-Correlation With $伪$ Abundances </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mazzola%2C+C+N">Christine N. Mazzola</a>, <a href="/search/astro-ph?searchtype=author&query=Badenes%2C+C">Carles Badenes</a>, <a href="/search/astro-ph?searchtype=author&query=Moe%2C+M">Maxwell Moe</a>, <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S+E">Sergey E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Kounkel%2C+M">Marina Kounkel</a>, <a href="/search/astro-ph?searchtype=author&query=Kratter%2C+K">Kaitlin Kratter</a>, <a href="/search/astro-ph?searchtype=author&query=Covey%2C+K">Kevin Covey</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+M+G">Matthew G. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+B">Brett Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Freeman%2C+P+E">Peter E. Freeman</a>, <a href="/search/astro-ph?searchtype=author&query=Anguiano%2C+B">Borja Anguiano</a>, <a href="/search/astro-ph?searchtype=author&query=Carlberg%2C+J+K">Joleen K. Carlberg</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lee%2C+N+M">Nathan M. De Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P+M">Peter M. Frinchaboy</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+H+M">Hannah M. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S">Steven Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D">David Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Price-Whelan%2C+A+M">Adrian M. Price-Whelan</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Troup%2C+N+W">Nicholas W. Troup</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.09059v2-abstract-short" style="display: inline;"> We use observations from the APOGEE survey to explore the relationship between stellar parameters and multiplicity. We combine high-resolution repeat spectroscopy for 41,363 dwarf and subgiant stars with abundance measurements from the APOGEE pipeline and distances and stellar parameters derived using \textit{Gaia} DR2 parallaxes from \cite{Sanders2018} to identify and characterise stellar multipl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.09059v2-abstract-full').style.display = 'inline'; document.getElementById('2007.09059v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.09059v2-abstract-full" style="display: none;"> We use observations from the APOGEE survey to explore the relationship between stellar parameters and multiplicity. We combine high-resolution repeat spectroscopy for 41,363 dwarf and subgiant stars with abundance measurements from the APOGEE pipeline and distances and stellar parameters derived using \textit{Gaia} DR2 parallaxes from \cite{Sanders2018} to identify and characterise stellar multiples with periods below 30 years, corresponding to \drvm$\gtrsim$ 3 \kms, where \drvm\ is the maximum APOGEE-detected shift in the radial velocities. Chemical composition is responsible for most of the variation in the close binary fraction in our sample, with stellar parameters like mass and age playing a secondary role. In addition to the previously identified strong anti-correlation between the close binary fraction and \feh\, we find that high abundances of $伪$ elements also suppress multiplicity at most values of \feh\ sampled by APOGEE. The anti-correlation between $伪$ abundances and multiplicity is substantially steeper than that observed for Fe, suggesting C, O, and Si in the form of dust and ices dominate the opacity of primordial protostellar disks and their propensity for fragmentation via gravitational stability. Near \feh{} = 0 dex, the bias-corrected close binary fraction ($a<10$ au) decreases from $\approx$ 100 per cent at \alh{} = $-$0.2 dex to $\approx$ 15 per cent near \alh{} = 0.08 dex, with a suggestive turn-up to $\approx$20 per cent near \alh{} = 0.2. We conclude that the relationship between stellar multiplicity and chemical composition for sun-like dwarf stars in the field of the Milky Way is complex, and that this complexity should be accounted for in future studies of interacting binaries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.09059v2-abstract-full').style.display = 'none'; document.getElementById('2007.09059v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 10 figures, plus appendices; accepted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.03687">arXiv:2007.03687</a> <span> [<a href="https://arxiv.org/pdf/2007.03687">pdf</a>, <a href="https://arxiv.org/format/2007.03687">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa2078">10.1093/mnras/staa2078 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The age-chemical abundance structure of the Galactic disc II: $伪$-dichotomy and thick disc formation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lian%2C+J">Jianhui Lian</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+D">Daniel Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Maraston%2C+C">Claudia Maraston</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">Christian Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Hern%C3%A1ndez%2C+D+A">D. A. Garc铆a-Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Munoz%2C+R+R">Ricardo R. Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+O">Olga Zamora</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.03687v2-abstract-short" style="display: inline;"> We extend our previous work on the age-chemical abundance structure of the Galactic outer disc to the inner disc (4 < r < 8 kpc) based on the SDSS/APOGEE survey. Different from the outer disc, the inner disc stars exhibit a clear bimodal distribution in the [Mg/Fe]-[Fe/H] plane. While a number of scenarios have been proposed in the literature, it remains challenging to recover this bimodal distrib… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.03687v2-abstract-full').style.display = 'inline'; document.getElementById('2007.03687v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.03687v2-abstract-full" style="display: none;"> We extend our previous work on the age-chemical abundance structure of the Galactic outer disc to the inner disc (4 < r < 8 kpc) based on the SDSS/APOGEE survey. Different from the outer disc, the inner disc stars exhibit a clear bimodal distribution in the [Mg/Fe]-[Fe/H] plane. While a number of scenarios have been proposed in the literature, it remains challenging to recover this bimodal distribution with theoretical models. To this end, we present a chemical evolution model embedding a complex multi-phase inner disc formation scenario that matches the observed bimodal [Mg/Fe]-[Fe/H] distribution. In this scenario, the formation of the inner disc is dominated by two main starburst episodes 6 Gyr apart with secular, low-level star formation activity in between. In our model, the first starburst occurs at early cosmic times (t~1 Gyr) and the second one 6 Gyr later at a cosmic time of t~7 Gyr. Both these starburst episodes are associated with gas accretion events in our model, and are quenched rapidly. The first starburst leads to the formation of the high-$伪$ sequence, and the second starburst leads to the formation of the metal-poor low-$伪$ sequence. The metal-rich low-$伪$ stars, instead, form during the secular evolution phase between the two bursts. Our model shows that the $伪$-dichotomy originates from the rapid suppression of star formation after the first starburst. The two starburst episodes are likely to be responsible for the formation of the geometric thick disc (z >1 kpc), with the old inner thick disc and the young outer thick disc forming during the first and the second starbursts, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.03687v2-abstract-full').style.display = 'none'; document.getElementById('2007.03687v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 10 figures. MNRAS in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.04263">arXiv:2004.04263</a> <span> [<a href="https://arxiv.org/pdf/2004.04263">pdf</a>, <a href="https://arxiv.org/format/2004.04263">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa1905">10.1093/mnras/staa1905 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Strong chemical tagging with APOGEE: 21 candidate star clusters that have dissolved across the Milky Way disc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Price-Jones%2C+N">Natalie Price-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Bovy%2C+J">Jo Bovy</a>, <a href="/search/astro-ph?searchtype=author&query=Webb%2C+J+J">Jeremy J. Webb</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachael Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Brownstein%2C+J+R">Joel R. Brownstein</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Donor%2C+J">John Donor</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P+M">Peter M. Frinchaboy</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Hern%C3%A1ndez%2C+D+A">D. A. Garc铆a-Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D+L">David L. Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2004.04263v2-abstract-short" style="display: inline;"> Chemically tagging groups of stars born in the same birth cluster is a major goal of spectroscopic surveys. To investigate the feasibility of such strong chemical tagging, we perform a blind chemical tagging experiment on abundances measured from APOGEE survey spectra. We apply a density-based clustering algorithm to the eight dimensional chemical space defined by [Mg/Fe], [Al/Fe], [Si/Fe], [K/Fe]… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.04263v2-abstract-full').style.display = 'inline'; document.getElementById('2004.04263v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.04263v2-abstract-full" style="display: none;"> Chemically tagging groups of stars born in the same birth cluster is a major goal of spectroscopic surveys. To investigate the feasibility of such strong chemical tagging, we perform a blind chemical tagging experiment on abundances measured from APOGEE survey spectra. We apply a density-based clustering algorithm to the eight dimensional chemical space defined by [Mg/Fe], [Al/Fe], [Si/Fe], [K/Fe], [Ti/Fe], [Mn/Fe], [Fe/H], and [Ni/Fe], abundances ratios which together span multiple nucleosynthetic channels. In a high quality sample of 182,538 giant stars, we detect twenty-one candidate clusters with more than fifteen members. Our candidate clusters are more chemically homogeneous than a population of non-member stars with similar [Mg/Fe] and [Fe/H], even in abundances not used for tagging. Group members are consistent with having the same age and fall along a single stellar-population track in logg vs. Teff space. Each group's members are distributed over multiple kpc, and the spread in their radial and azimuthal actions increases with age. We qualitatively reproduce this increase using N-body simulations of cluster dissolution in Galactic potentials that include transient winding spiral arms. Observing our candidate birth clusters with high-resolution spectroscopy in other wavebands to investigate their chemical homogeneity in other nucleosynthetic groups will be essential to confirming the efficacy of strong chemical tagging. Our initially spatially-compact but now widely dispersed candidate clusters will provide novel limits on chemical evolution and orbital diffusion in the Galactic disc, and constraints on star formation in loosely-bound groups. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.04263v2-abstract-full').style.display = 'none'; document.getElementById('2004.04263v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 9 figures, accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.09469">arXiv:2003.09469</a> <span> [<a href="https://arxiv.org/pdf/2003.09469">pdf</a>, <a href="https://arxiv.org/format/2003.09469">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab8127">10.3847/1538-4357/ab8127 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectral classification of B stars: The empirical sequence using SDSS-IV/APOGEE near-IR data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez-Preciado%2C+V+G">Valeria G. Ram铆rez-Preciado</a>, <a href="/search/astro-ph?searchtype=author&query=Rom%C3%A1n-L%C3%B3pes%2C+A">Alexandre Rom谩n-L贸pes</a>, <a href="/search/astro-ph?searchtype=author&query=Rom%C3%A1n-Zu%C3%B1iga%2C+C+G">Carlos G. Rom谩n-Zu帽iga</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez%2C+J">Jes煤s Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+A">Anibal Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K">Keivan Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Stringfellow%2C+G+S">Guy S. Stringfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J+S">Jinyoung Serena Kim</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2003.09469v1-abstract-short" style="display: inline;"> We present a semi-empirical spectral classification scheme for normal B-type stars using near-infrared spectra (1.5-1.7 $渭$m) from the SDSS APOGEE2-N DR14 database. The main motivation for working with B-type stars is their importance in the evolution of young stellar clusters, however we also take advantage of having a numerous sample (316 stars) of B-type star candidates in APOGEE2-N, for which… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.09469v1-abstract-full').style.display = 'inline'; document.getElementById('2003.09469v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.09469v1-abstract-full" style="display: none;"> We present a semi-empirical spectral classification scheme for normal B-type stars using near-infrared spectra (1.5-1.7 $渭$m) from the SDSS APOGEE2-N DR14 database. The main motivation for working with B-type stars is their importance in the evolution of young stellar clusters, however we also take advantage of having a numerous sample (316 stars) of B-type star candidates in APOGEE2-N, for which we also have optical (3600-9100 \angstrom) counterparts from the LAMOST survey. By first obtaining an accurate spectral classification of the sources using the LAMOST DR3 spectra and the canonical spectral classification scheme Gray & Corbally 2009, we found a linear relation between optical spectral types and the equivalent widths of the hydrogen lines of the Brackett series in the APOGEE2-N NIR spectra. This relation extends smoothly from a similar relation for O and early-B stars found by Roman-Lopes et al. (2018). This way, we obtain a catalog of B-type sources with features in both the optical and NIR, and a classification scheme refined down to one spectral sub-class. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.09469v1-abstract-full').style.display = 'none'; document.getElementById('2003.09469v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures and 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.08980">arXiv:2002.08980</a> <span> [<a href="https://arxiv.org/pdf/2002.08980">pdf</a>, <a href="https://arxiv.org/format/2002.08980">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ab77bc">10.3847/1538-3881/ab77bc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Open Cluster Chemical Abundances and Mapping Survey: IV. Abundances for 128 Open Clusters using SDSS/APOGEE DR16 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Donor%2C+J">John Donor</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P+M">Peter M. Frinchaboy</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Connell%2C+J+E">Julia E. O'Connell</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+A">Andres Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Anders%2C+F">Friedrich Anders</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachael Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Bizyaev%2C+D">Dmitry Bizyaev</a>, <a href="/search/astro-ph?searchtype=author&query=Brownstein%2C+J+R">Joel R. Brownstein</a>, <a href="/search/astro-ph?searchtype=author&query=Carrera%2C+R">Ricardo Carrera</a>, <a href="/search/astro-ph?searchtype=author&query=Chiappini%2C+C">Cristina Chiappini</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R">Roger Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Hernandez%2C+D+A">D. A. Garcia-Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=Jonsson%2C+H">Henrik Jonsson</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">Christian Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+K">Kaike Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Sobeck%2C+J+S">Jennifer S. Sobeck</a>, <a href="/search/astro-ph?searchtype=author&query=Zasowski%2C+G">Gail Zasowski</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2002.08980v1-abstract-short" style="display: inline;"> The Open Cluster Chemical Abundances and Mapping (OCCAM) survey aims to constrain key Galactic dynamical and chemical evolution parameters by the construction of a large, comprehensive, uniform, infrared-based spectroscopic data set of hundreds of open clusters. This fourth contribution from the OCCAM survey presents analysis using SDSS/APOGEE DR16 of a sample of 128 open clusters, 71 of which we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.08980v1-abstract-full').style.display = 'inline'; document.getElementById('2002.08980v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.08980v1-abstract-full" style="display: none;"> The Open Cluster Chemical Abundances and Mapping (OCCAM) survey aims to constrain key Galactic dynamical and chemical evolution parameters by the construction of a large, comprehensive, uniform, infrared-based spectroscopic data set of hundreds of open clusters. This fourth contribution from the OCCAM survey presents analysis using SDSS/APOGEE DR16 of a sample of 128 open clusters, 71 of which we designate to be "high quality" based on the appearance of their color-magnitude diagram. We find the APOGEE DR16 derived [Fe/H] abundances to be in good agreement with previous high resolution spectroscopic open cluster abundance studies. Using the high quality sample, we measure Galactic abundance gradients in 16 elements, and find evolution of some of the [X/Fe] gradients as a function of age. We find an overall Galactic [Fe/H] vs R_GC gradient of $-0.068 \pm 0.001$ dex kpc$^{-1}$ over the range of $6 <$ R_GC $< 13.9$ kpc; however, we note that this result is sensitive to the distance catalog used, varying as much as 15%. We formally derive the location a break in the [Fe/H] abundance gradient as a free parameter in the gradient fit for the first time. We also measure significant Galactic gradients in O, Mg, S, Ca, Mn, Cr, Cu, Na, Al, and K, some of which are measured for the first time. Our large sample allows us to explore four well-populated age bins to explore the time evolution of gradients for a large number of elements and comment on possible implications for Galactic chemical evolution and radial migration. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.08980v1-abstract-full').style.display = 'none'; document.getElementById('2002.08980v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 14 figures, Accepted for publication by AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.03177">arXiv:2001.03177</a> <span> [<a href="https://arxiv.org/pdf/2001.03177">pdf</a>, <a href="https://arxiv.org/format/2001.03177">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa478">10.1093/mnras/staa478 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Chemical Compositions of Accreted and {\it in situ} Galactic Globular Clusters According to SDSS/APOGEE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Horta%2C+D">Danny Horta</a>, <a href="/search/astro-ph?searchtype=author&query=Schiavon%2C+R+P">Ricardo P. Schiavon</a>, <a href="/search/astro-ph?searchtype=author&query=Mackereth%2C+J+T">J. Ted Mackereth</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P+M">Peter M. Frinchaboy</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Hern%C3%A1ndez%2C+D+A">D. A. Garc铆a-Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselquist%2C+S">Sten Hasselquist</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B6nsson%2C+H">Henrik J枚nsson</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">Richard R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9sz%C3%A1ros%2C+S">Szabolcs M茅sz谩ros</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">Christian Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Nataf%2C+D+M">David M. Nataf</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Vargas-Gonz%C3%A1lez%2C+J">Jaime Vargas-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Zasowski%2C+G">Gail Zasowski</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.03177v4-abstract-short" style="display: inline;"> Studies of the kinematics and chemical compositions of Galactic globular clusters (GCs) enable the reconstruction of the history of star formation, chemical evolution, and mass assembly of the Galaxy. Using the latest data release (DR16) of the SDSS/APOGEE survey, we identify 3,090 stars associated with 46 GCs. Using a previously defined kinematic association, we break the sample down into eight s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.03177v4-abstract-full').style.display = 'inline'; document.getElementById('2001.03177v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.03177v4-abstract-full" style="display: none;"> Studies of the kinematics and chemical compositions of Galactic globular clusters (GCs) enable the reconstruction of the history of star formation, chemical evolution, and mass assembly of the Galaxy. Using the latest data release (DR16) of the SDSS/APOGEE survey, we identify 3,090 stars associated with 46 GCs. Using a previously defined kinematic association, we break the sample down into eight separate groups and examine how the kinematics-based classification maps into chemical composition space, considering only $伪$ (mostly Si and Mg) elements and Fe. Our results show that: (i) The loci of both in situ and accreted subgroups in chemical space match those of their field counterparts; (ii) GCs from different individual accreted subgroups occupy the same locus in chemical space. This could either mean that they share a similar origin or that they are associated with distinct satellites which underwent similar chemical enrichment histories; (iii) The chemical compositions of the GCs associated with the low orbital energy subgroup defined by Massari and collaborators is broadly consistent with an in situ origin. However, at the low metallicity end, the distinction between accreted and in situ populations is blurred; (iv) Regarding the status of GCs whose origin is ambiguous, we conclude the following: the position in Si-Fe plane suggests an in situ}origin for Liller 1 and a likely accreted origin for NGC 5904 and NGC 6388. The case of NGC 288 is unclear, as its orbital properties suggest an accretion origin, its chemical composition suggests it may have formed in situ. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.03177v4-abstract-full').style.display = 'none'; document.getElementById('2001.03177v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 10 figures, 3 tables. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.00431">arXiv:2001.00431</a> <span> [<a href="https://arxiv.org/pdf/2001.00431">pdf</a>, <a href="https://arxiv.org/format/2001.00431">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab9596">10.3847/1538-4357/ab9596 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Wolf-Rayet galaxies in SDSS-IV MaNGA. I. Catalog construction and sample properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liang%2C+F">Fu-Heng Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+C">Cheng Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+N">Niu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+R">Renbin Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Mo%2C+H">Houjun Mo</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+W">Wei Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Machuca%2C+C">Camilo Machuca</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.00431v2-abstract-short" style="display: inline;"> Wolf-Rayet (WR) galaxies are a rare population of galaxies that host living high-mass stars during their WR phase (i.e. WR stars) and are thus expected to provide interesting constraints on the stellar Initial Mass Function, massive star formation, stellar evolution models, etc. Spatially resolved spectroscopy should in principle provide a more efficient way of identifying WR galaxies than single-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.00431v2-abstract-full').style.display = 'inline'; document.getElementById('2001.00431v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.00431v2-abstract-full" style="display: none;"> Wolf-Rayet (WR) galaxies are a rare population of galaxies that host living high-mass stars during their WR phase (i.e. WR stars) and are thus expected to provide interesting constraints on the stellar Initial Mass Function, massive star formation, stellar evolution models, etc. Spatially resolved spectroscopy should in principle provide a more efficient way of identifying WR galaxies than single-fiber surveys of galactic centers such as SDSS-I & II, as WR stars should be more preferentially found in discs. Using IFU data from the ongoing SDSS-IV MaNGA survey, we have performed a thorough search for WR galaxies. We first identify H II regions in each datacube and carry out full spectral fitting to the stacked spectra. We then visually inspect the residual spectrum of each H II region and identify WR regions that present a significant "blue bump" at 4600-4750 A. The resulting WR catalog includes 267 WR regions of ~500pc (radius) sizes, distributed in 90 galaxies from the current sample of MaNGA (MaNGA Product Launch 7). We find WR regions are exclusively found in galaxies that show bluest colors and highest star formation rates for their mass. Most WR galaxies have late-type morphologies and show relatively large asymmetry in their images, implying that WR regions are more preferentially found in interacting/merging galaxies. We estimate the stellar mass function of WR galaxies and the mass-dependent detection rate. The detection rate of WR galaxies is typically ~2%, with weak dependence on stellar mass. This detection rate is about 40 times higher than previous studies with SDSS single fiber data, and by a factor of 2 lower than the CALIFA-based WR catalog. We make comparisons with SDSS and CALIFA studies, and conclude that different detection rates can be explained mainly by three factors: spatial coverage, spectral signal-to-noise ratio, and redshift ranges of the parent sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.00431v2-abstract-full').style.display = 'none'; document.getElementById('2001.00431v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 12 figures, 2 tables; Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.09778">arXiv:1912.09778</a> <span> [<a href="https://arxiv.org/pdf/1912.09778">pdf</a>, <a href="https://arxiv.org/format/1912.09778">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201937364">10.1051/0004-6361/201937364 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> From the bulge to the outer disc: StarHorse stellar parameters, distances, and extinctions for stars in APOGEE DR16 and other spectroscopic surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Queiroz%2C+A+B+A">A. B. A. Queiroz</a>, <a href="/search/astro-ph?searchtype=author&query=Anders%2C+F">F. Anders</a>, <a href="/search/astro-ph?searchtype=author&query=Chiappini%2C+C">C. Chiappini</a>, <a href="/search/astro-ph?searchtype=author&query=Khalatyan%2C+A">A. Khalatyan</a>, <a href="/search/astro-ph?searchtype=author&query=Santiago%2C+B+X">B. X. Santiago</a>, <a href="/search/astro-ph?searchtype=author&query=Steinmetz%2C+M">M. Steinmetz</a>, <a href="/search/astro-ph?searchtype=author&query=Valentini%2C+M">M. Valentini</a>, <a href="/search/astro-ph?searchtype=author&query=Miglio%2C+A">A. Miglio</a>, <a href="/search/astro-ph?searchtype=author&query=Bossini%2C+D">D. Bossini</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Minchev%2C+I">I. Minchev</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+D+A+G">D. A. Garc铆a Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Schultheis%2C+M">M. Schultheis</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">R. L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">T. C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Bizyaev%2C+D">D. Bizyaev</a>, <a href="/search/astro-ph?searchtype=author&query=Brownstein%2C+J+R">J. R. Brownstein</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">K. Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">J. G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P+M">P. M. Frinchaboy</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">R. R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">S. R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Nataf%2C+D">D. Nataf</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">C. Nitschelm</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1912.09778v3-abstract-short" style="display: inline;"> We combine high-resolution spectroscopic data from APOGEE-2 Survey Data Release 16 (DR16) with broad-band photometric data from several sources, as well as parallaxes from {\it Gaia} Data Release 2 (DR2). Using the Bayesian isochrone-fitting code {\tt StarHorse}, we derive distances, extinctions and astrophysical parameters for around 388,815 APOGEE stars, achieving typical distance uncertainties… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.09778v3-abstract-full').style.display = 'inline'; document.getElementById('1912.09778v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.09778v3-abstract-full" style="display: none;"> We combine high-resolution spectroscopic data from APOGEE-2 Survey Data Release 16 (DR16) with broad-band photometric data from several sources, as well as parallaxes from {\it Gaia} Data Release 2 (DR2). Using the Bayesian isochrone-fitting code {\tt StarHorse}, we derive distances, extinctions and astrophysical parameters for around 388,815 APOGEE stars, achieving typical distance uncertainties of $\sim 6\%$ for APOGEE giants, $\sim 2\%$ for APOGEE dwarfs, as well as extinction uncertainties of $\sim 0.07$ mag when all photometric information is available, and $\sim 0.17$ mag if optical photometry is missing. {\tt StarHorse} uncertainties vary with the input spectroscopic catalogue, with the available photometry, and with the parallax uncertainties. To illustrate the impact of our results, we show that, thanks to {\it Gaia} DR2 and the now larger sky coverage of APOGEE-2 (including APOGEE-South), we obtain an extended map of the Galactic plane, providing unprecedented coverage of the disk close to the Galactic mid-plane ($|Z_{Gal}|<1$ kpc) from the Galactic Centre out to $R_{\rm Gal}\sim 20$ kpc. The improvements in statistics as well as distance and extinction uncertainties unveil the presence of the bar in stellar density, as well as the striking chemical duality in the innermost regions of the disk, now clearly extending to the inner bulge. We complement this paper with distances and extinctions for stars in other public released spectroscopic surveys: 324,999 in GALAH DR2, 4,928,715 in LAMOST DR5, 408,894 in RAVE DR6, and 6,095 in GES DR3 <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.09778v3-abstract-full').style.display = 'none'; document.getElementById('1912.09778v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to A&A. 17 pages, 11 figures. Data products are available at https://data.aip.de/aqueiroz2020, (doi:10.17876/data/2020_2)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 638, A76 (2020) </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Roman-Lopes%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Roman-Lopes%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Roman-Lopes%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Roman-Lopes%2C+A&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> 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