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<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=Blum%2C+R&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Blum%2C+R&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Blum%2C+R&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Blum%2C+R&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/2501.10759">arXiv:2501.10759</a> <span> [<a href="https://arxiv.org/pdf/2501.10759">pdf</a>, <a href="https://arxiv.org/format/2501.10759">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Studying baryon acoustic oscillations using photometric redshifts from the DESI Legacy Imaging survey DR9 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saulder%2C+C">Christoph Saulder</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yong-Seon Song</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+M">Minji Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+Y">Yi Zheng</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=Zhou%2C+R">Rongpu Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+J+A">Jeffrey A. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Chuang%2C+C">Chia-Hsun Chuang</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">Jessica Nicole Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">Biprateep Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Z">Zhejie Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">Peter Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">Enrique Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">Satya Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">Gaston Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">Stephanie Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Kirkby%2C+D">David Kirkby</a>, <a href="/search/astro-ph?searchtype=author&query=Kisner%2C+T">Theodore Kisner</a>, <a href="/search/astro-ph?searchtype=author&query=Kremin%2C+A">Anthony Kremin</a> , et al. (19 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="2501.10759v2-abstract-short" style="display: inline;"> Context.The Dark Energy Spectroscopic Instrument (DESI) Legacy Imaging Survey DR9 (DR9 hereafter), with its extensive dataset of galaxy locations and photometric redshifts, presents an opportunity to study baryon acoustic oscillations (BAOs) in the region covered by the ongoing spectroscopic survey with DESI. Aims. We aim to investigate differences between different parts of the DR9 footprint. F… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.10759v2-abstract-full').style.display = 'inline'; document.getElementById('2501.10759v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.10759v2-abstract-full" style="display: none;"> Context.The Dark Energy Spectroscopic Instrument (DESI) Legacy Imaging Survey DR9 (DR9 hereafter), with its extensive dataset of galaxy locations and photometric redshifts, presents an opportunity to study baryon acoustic oscillations (BAOs) in the region covered by the ongoing spectroscopic survey with DESI. Aims. We aim to investigate differences between different parts of the DR9 footprint. Furthermore, we want to measure the BAO scale for luminous red galaxies within them. Our selected redshift range of 0.6 to 0.8 corresponds to the bin in which a tension between DESI Y1 and eBOSS was found. Methods. We calculated the anisotropic two-point correlation function in a modified binning scheme to detect the BAOs in DR9 data. We then used template fits based on simulations to measure the BAO scale in the imaging data. Results. Our analysis reveals the expected correlation function shape in most of the footprint areas, showing a BAO scale consistent with Planck's observations. Aside from identified mask-related data issues in the southern region of the South Galactic Cap, we find a notable variance between the different footprints. Conclusions. We find that this variance is consistent with the difference between the DESI Y1 and eBOSS data, and it supports the argument that that tension is caused by sample variance. Additionally, we also uncovered systematic biases not previously accounted for in photometric BAO studies. We emphasize the necessity of adjusting for the systematic shift in the BAO scale associated with typical photometric redshift uncertainties to ensure accurate measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.10759v2-abstract-full').style.display = 'none'; document.getElementById('2501.10759v2-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> 9 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </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">14 pages, 14 figures, 3 tables, accepted in Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.12022">arXiv:2411.12022</a> <span> [<a href="https://arxiv.org/pdf/2411.12022">pdf</a>, <a href="https://arxiv.org/format/2411.12022">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Bahr-Kalus%2C+B">B. Bahr-Kalus</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a> , et al. (188 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="2411.12022v2-abstract-short" style="display: inline;"> We present cosmological results from the measurement of clustering of galaxy, quasar and Lyman-$伪$ forest tracers from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). We adopt the full-shape (FS) modeling of the power spectrum, including the effects of redshift-space distortions, in an analysis which has been validated in a series of supporting p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12022v2-abstract-full').style.display = 'inline'; document.getElementById('2411.12022v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12022v2-abstract-full" style="display: none;"> We present cosmological results from the measurement of clustering of galaxy, quasar and Lyman-$伪$ forest tracers from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). We adopt the full-shape (FS) modeling of the power spectrum, including the effects of redshift-space distortions, in an analysis which has been validated in a series of supporting papers. In the flat $螞$CDM cosmological model, DESI (FS+BAO), combined with a baryon density prior from Big Bang Nucleosynthesis and a weak prior on the scalar spectral index, determines matter density to $惟_\mathrm{m}=0.2962\pm 0.0095$, and the amplitude of mass fluctuations to $蟽_8=0.842\pm 0.034$. The addition of the cosmic microwave background (CMB) data tightens these constraints to $惟_\mathrm{m}=0.3056\pm 0.0049$ and $蟽_8=0.8121\pm 0.0053$, while further addition of the the joint clustering and lensing analysis from the Dark Energy Survey Year-3 (DESY3) data leads to a 0.4% determination of the Hubble constant, $H_0 = (68.40\pm 0.27)\,{\rm km\,s^{-1}\,Mpc^{-1}}$. In models with a time-varying dark energy equation of state, combinations of DESI (FS+BAO) with CMB and type Ia supernovae continue to show the preference, previously found in the DESI DR1 BAO analysis, for $w_0>-1$ and $w_a<0$ with similar levels of significance. DESI data, in combination with the CMB, impose the upper limits on the sum of the neutrino masses of $\sum m_谓< 0.071\,{\rm eV}$ at 95% confidence. DESI data alone measure the modified-gravity parameter that controls the clustering of massive particles, $渭_0=0.11^{+0.45}_{-0.54}$, while the combination of DESI with the CMB and the clustering and lensing analysis from DESY3 constrains both modified-gravity parameters, giving $渭_0 = 0.04\pm 0.22$ and $危_0 = 0.044\pm 0.047$, in agreement with general relativity. [Abridged.] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12022v2-abstract-full').style.display = 'none'; document.getElementById('2411.12022v2-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/). 55 pages, 10 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/2411.12021">arXiv:2411.12021</a> <span> [<a href="https://arxiv.org/pdf/2411.12021">pdf</a>, <a href="https://arxiv.org/format/2411.12021">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a> , et al. (174 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="2411.12021v2-abstract-short" style="display: inline;"> We present the measurements and cosmological implications of the galaxy two-point clustering using over 4.7 million unique galaxy and quasar redshifts in the range $0.1<z<2.1$ divided into six redshift bins over a $\sim 7,500$ square degree footprint, from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). By fitting the full power spectrum, we exte… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12021v2-abstract-full').style.display = 'inline'; document.getElementById('2411.12021v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12021v2-abstract-full" style="display: none;"> We present the measurements and cosmological implications of the galaxy two-point clustering using over 4.7 million unique galaxy and quasar redshifts in the range $0.1<z<2.1$ divided into six redshift bins over a $\sim 7,500$ square degree footprint, from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). By fitting the full power spectrum, we extend previous DESI DR1 baryon acoustic oscillation (BAO) measurements to include redshift-space distortions and signals from the matter-radiation equality scale. For the first time, this Full-Shape analysis is blinded at the catalogue-level to avoid confirmation bias and the systematic errors are accounted for at the two-point clustering level, which automatically propagates them into any cosmological parameter. When analysing the data in terms of compressed model-agnostic variables, we obtain a combined precision of 4.7\% on the amplitude of the redshift space distortion signal reaching similar precision with just one year of DESI data than with 20 years of observation from previous generation surveys. We analyse the data to directly constrain the cosmological parameters within the $螞$CDM model using perturbation theory and combine this information with the reconstructed DESI DR1 galaxy BAO. Using a Big Bang Nucleosynthesis Gaussian prior on the baryon density parameter, and a Gaussian prior on the spectral index, we constrain the matter density is $惟_m=0.296\pm 0.010 $ and the Hubble constant $H_0=(68.63 \pm 0.79)[{\rm km\, s^{-1}Mpc^{-1}}]$. Additionally, we measure the amplitude of clustering $蟽_8=0.841 \pm 0.034$. The DESI DR1 results are in agreement with the $螞$CDM model based on general relativity with parameters consistent with those from Planck. The cosmological interpretation of these results in combination with external datasets are presented in a companion paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12021v2-abstract-full').style.display = 'none'; document.getElementById('2411.12021v2-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/). 76 pages, 20 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/2411.12020">arXiv:2411.12020</a> <span> [<a href="https://arxiv.org/pdf/2411.12020">pdf</a>, <a href="https://arxiv.org/format/2411.12020">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> DESI 2024 II: Sample Definitions, Characteristics, and Two-point Clustering Statistics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a> , et al. (178 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="2411.12020v1-abstract-short" style="display: inline;"> We present the samples of galaxies and quasars used for DESI 2024 cosmological analyses, drawn from the DESI Data Release 1 (DR1). We describe the construction of large-scale structure (LSS) catalogs from these samples, which include matched sets of synthetic reference `randoms' and weights that account for variations in the observed density of the samples due to experimental design and varying in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12020v1-abstract-full').style.display = 'inline'; document.getElementById('2411.12020v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12020v1-abstract-full" style="display: none;"> We present the samples of galaxies and quasars used for DESI 2024 cosmological analyses, drawn from the DESI Data Release 1 (DR1). We describe the construction of large-scale structure (LSS) catalogs from these samples, which include matched sets of synthetic reference `randoms' and weights that account for variations in the observed density of the samples due to experimental design and varying instrument performance. We detail how we correct for variations in observational completeness, the input `target' densities due to imaging systematics, and the ability to confidently measure redshifts from DESI spectra. We then summarize how remaining uncertainties in the corrections can be translated to systematic uncertainties for particular analyses. We describe the weights added to maximize the signal-to-noise of DESI DR1 2-point clustering measurements. We detail measurement pipelines applied to the LSS catalogs that obtain 2-point clustering measurements in configuration and Fourier space. The resulting 2-point measurements depend on window functions and normalization constraints particular to each sample, and we present the corrections required to match models to the data. We compare the configuration- and Fourier-space 2-point clustering of the data samples to that recovered from simulations of DESI DR1 and find they are, generally, in statistical agreement to within 2\% in the inferred real-space over-density field. The LSS catalogs, 2-point measurements, and their covariance matrices will be released publicly with DESI DR1. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12020v1-abstract-full').style.display = 'none'; document.getElementById('2411.12020v1-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> 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.03996">arXiv:2408.03996</a> <span> [<a href="https://arxiv.org/pdf/2408.03996">pdf</a>, <a href="https://arxiv.org/format/2408.03996">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"> The atomic gas sequence and mass-metallicity relation from dwarfs to massive galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scholte%2C+D">D. Scholte</a>, <a href="/search/astro-ph?searchtype=author&query=Saintonge%2C+A">A. Saintonge</a>, <a href="/search/astro-ph?searchtype=author&query=Moustakas%2C+J">J. Moustakas</a>, <a href="/search/astro-ph?searchtype=author&query=Catinella%2C+B">B. Catinella</a>, <a href="/search/astro-ph?searchtype=author&query=Zou%2C+H">H. Zou</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">B. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Circosta%2C+C">C. Circosta</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%B6rster%2C+P+U">P. U. F枚rster</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">S. Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">R. Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Kisner%2C+T">T. Kisner</a>, <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S+E">S. E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Kremin%2C+A">A. Kremin</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="2408.03996v1-abstract-short" style="display: inline;"> Galaxy scaling relations provide insights into the processes that drive galaxy evolution. The extension of these scaling relations into the dwarf galaxy regime is of particular interest. This is because dwarf galaxies represent a crucial stage in galaxy evolution, and understanding them could also shed light on their role in reionising the early Universe. There is currently no consensus on the pro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03996v1-abstract-full').style.display = 'inline'; document.getElementById('2408.03996v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.03996v1-abstract-full" style="display: none;"> Galaxy scaling relations provide insights into the processes that drive galaxy evolution. The extension of these scaling relations into the dwarf galaxy regime is of particular interest. This is because dwarf galaxies represent a crucial stage in galaxy evolution, and understanding them could also shed light on their role in reionising the early Universe. There is currently no consensus on the processes that dominate the evolution of dwarfs. In this work we constrain the atomic gas sequence (stellar mass vs. atomic gas fraction) and mass-metallicity relation (stellar mass vs. gas phase metallicity) from dwarf ($10^{6.5}$ $\textrm{M}_{\odot}$) to massive ($10^{11.5}$ $\textrm{M}_{\odot}$) galaxies in the local Universe. The combined optical and 21-cm spectroscopic observations of the DESI and ALFALFA surveys allow us to simultaneously constrain both scaling relations. We find a slope change of the atomic gas sequence at a stellar mass of $\sim 10^{9} ~\textrm{M}_{\odot}$. We also find that the shape and scatter of the atomic gas sequence and mass-metallicity relation are strongly linked for both dwarfs and more massive galaxies. Consequently, the low mass slope change of the atomic gas sequence is imprinted onto the mass-metallicity relation of dwarf galaxies. The mass scale of the measured slope change is consistent with a predicted escape velocity threshold below which low mass galaxies experience significant supernova-driven gas loss, as well as with a reduction in cold gas accretion onto more massive galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03996v1-abstract-full').style.display = 'none'; document.getElementById('2408.03996v1-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> 7 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">16 pages, 10 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/2407.06280">arXiv:2407.06280</a> <span> [<a href="https://arxiv.org/pdf/2407.06280">pdf</a>, <a href="https://arxiv.org/format/2407.06280">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> <p class="title is-5 mathjax"> DESI Early Data Release Milky Way Survey Value-Added Catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S+E">Sergey E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Allende-Prieto%2C+C">C. Allende-Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+A+P">A. P. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+T+S">T. S. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+L+B+e">L. Beraldo e Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+B">B. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Carrillo%2C+A">A. Carrillo</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">A. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Manser%2C+C+J">C. J. Manser</a>, <a href="/search/astro-ph?searchtype=author&query=Nikakhtar%2C+F">F. Nikakhtar</a>, <a href="/search/astro-ph?searchtype=author&query=Riley%2C+A+H">A. H. Riley</a>, <a href="/search/astro-ph?searchtype=author&query=Rockosi%2C+C">C. Rockosi</a>, <a href="/search/astro-ph?searchtype=author&query=Valluri%2C+M">M. Valluri</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">B. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+J">J. Guy</a> , et al. (18 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="2407.06280v2-abstract-short" style="display: inline;"> We present the stellar value-added catalogue based on the Dark Energy Spectroscopic Instrument (DESI) Early Data Release. The catalogue contains radial velocity and stellar parameter measurements for $\simeq$ 400,000 unique stars observed during commissioning and survey validation by DESI. These observations were made under conditions similar to the Milky Way Survey (MWS) currently carried out by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.06280v2-abstract-full').style.display = 'inline'; document.getElementById('2407.06280v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.06280v2-abstract-full" style="display: none;"> We present the stellar value-added catalogue based on the Dark Energy Spectroscopic Instrument (DESI) Early Data Release. The catalogue contains radial velocity and stellar parameter measurements for $\simeq$ 400,000 unique stars observed during commissioning and survey validation by DESI. These observations were made under conditions similar to the Milky Way Survey (MWS) currently carried out by DESI but also include multiple specially targeted fields, such as those containing well-studied dwarf galaxies and stellar streams. The majority of observed stars have $16<r<20$ with a median signal-to-noise ratio in the spectra of $\sim$ 20. In the paper, we describe the structure of the catalogue, give an overview of different target classes observed, as well as provide recipes for selecting clean stellar samples. We validate the catalogue using external high-resolution measurements and show that radial velocities, surface gravities, and iron abundances determined by DESI are accurate to 1 km/s, $0.3$ dex and $\sim$ 0.15 dex respectively. We also demonstrate possible uses of the catalogue for chemo-dynamical studies of the Milky Way stellar halo and Draco dwarf spheroidal. The value-added catalogue described in this paper is the very first DESI MWS catalogue. The next DESI data release, expected in less than a year, will add the data from the first year of DESI survey operations and will contain approximately 4 million stars, along with significant processing improvements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.06280v2-abstract-full').style.display = 'none'; document.getElementById('2407.06280v2-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">Accepted to MNRAS; Value added catalogue is available at https://data.desi.lbl.gov/public/edr/vac/edr/mws/fuji/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03123">arXiv:2404.03123</a> <span> [<a href="https://arxiv.org/pdf/2404.03123">pdf</a>, <a href="https://arxiv.org/format/2404.03123">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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"> Constraints on the spacetime variation of the fine-structure constant using DESI emission-line galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+L">Linhua Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Z">Zhiwei Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">Jessica Nicole Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">Peter Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">Kevin Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gaztanaga%2C+E">Enrique Gaztanaga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">Satya Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">Gaston Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">Klaus Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">Stephanie Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Landriau%2C+M">Martin Landriau</a>, <a href="/search/astro-ph?searchtype=author&query=Guillou%2C+L+L">Laurent Le Guillou</a>, <a href="/search/astro-ph?searchtype=author&query=Levi%2C+M">Michael Levi</a>, <a href="/search/astro-ph?searchtype=author&query=Manera%2C+M">Marc Manera</a>, <a href="/search/astro-ph?searchtype=author&query=Miquel%2C+R">Ramon Miquel</a>, <a href="/search/astro-ph?searchtype=author&query=Moustakas%2C+J">John Moustakas</a>, <a href="/search/astro-ph?searchtype=author&query=Mueller%2C+E">Eva-Maria Mueller</a> , et al. (16 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="2404.03123v2-abstract-short" style="display: inline;"> We present strong constraints on the spacetime variation of the fine-structure constant $伪$ using the Dark Energy Spectroscopic Instrument (DESI). In this pilot work, we utilize $\sim110,000$ galaxies with strong and narrow O III $位位$4959,5007 emission lines to measure the relative variation $螖伪/伪$ in space and time. The O III doublet is arguably the best choice for this purpose owing to its wide… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03123v2-abstract-full').style.display = 'inline'; document.getElementById('2404.03123v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03123v2-abstract-full" style="display: none;"> We present strong constraints on the spacetime variation of the fine-structure constant $伪$ using the Dark Energy Spectroscopic Instrument (DESI). In this pilot work, we utilize $\sim110,000$ galaxies with strong and narrow O III $位位$4959,5007 emission lines to measure the relative variation $螖伪/伪$ in space and time. The O III doublet is arguably the best choice for this purpose owing to its wide wavelength separation between the two lines and its strong emission in many galaxies. Our galaxy sample spans a redshift range of $0<z<0.95$, covering half of all cosmic time. We divide the sample into subsamples in 10 redshift bins ($螖z=0.1$), and calculate $螖伪/伪$ for the individual subsamples. The uncertainties of the measured $螖伪/伪$ are roughly between $2\times10^{-6}$ and $2\times10^{-5}$. We find an apparent $伪$ variation with redshift at a level of $螖伪/伪=(2\sim3)\times10^{-5}$. This is highly likely to be caused by systematics associated with wavelength calibration, since such small systematics can be caused by a wavelength distortion of $0.002-0.003$ 脜, which is beyond the accuracy that the current DESI data can achieve. We refine the wavelength calibration using sky lines for a small fraction of the galaxies, but it does not change our main results. We further probe the spatial variation of $伪$ in small redshift ranges, and do not find obvious, large-scale structures in the spatial distribution of $螖伪/伪$. As DESI is ongoing, we will include more galaxies, and by improving the wavelength calibration, we expect to obtain a better constraint that is comparable to the strongest current constraint. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03123v2-abstract-full').style.display = 'none'; document.getElementById('2404.03123v2-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">17 pages, 11 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/2404.03002">arXiv:2404.03002</a> <span> [<a href="https://arxiv.org/pdf/2404.03002">pdf</a>, <a href="https://arxiv.org/format/2404.03002">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Bahr-Kalus%2C+B">B. Bahr-Kalus</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Bera%2C+A">A. Bera</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a> , et al. (178 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="2404.03002v3-abstract-short" style="display: inline;"> We present cosmological results from the measurement of baryon acoustic oscillations (BAO) in galaxy, quasar and Lyman-$伪$ forest tracers from the first year of observations from the Dark Energy Spectroscopic Instrument (DESI), to be released in the DESI Data Release 1. DESI BAO provide robust measurements of the transverse comoving distance and Hubble rate, or their combination, relative to the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03002v3-abstract-full').style.display = 'inline'; document.getElementById('2404.03002v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03002v3-abstract-full" style="display: none;"> We present cosmological results from the measurement of baryon acoustic oscillations (BAO) in galaxy, quasar and Lyman-$伪$ forest tracers from the first year of observations from the Dark Energy Spectroscopic Instrument (DESI), to be released in the DESI Data Release 1. DESI BAO provide robust measurements of the transverse comoving distance and Hubble rate, or their combination, relative to the sound horizon, in seven redshift bins from over 6 million extragalactic objects in the redshift range $0.1<z<4.2$. DESI BAO data alone are consistent with the standard flat $螞$CDM cosmological model with a matter density $惟_\mathrm{m}=0.295\pm 0.015$. Paired with a BBN prior and the robustly measured acoustic angular scale from the CMB, DESI requires $H_0=(68.52\pm0.62)$ km/s/Mpc. In conjunction with CMB anisotropies from Planck and CMB lensing data from Planck and ACT, we find $惟_\mathrm{m}=0.307\pm 0.005$ and $H_0=(67.97\pm0.38)$ km/s/Mpc. Extending the baseline model with a constant dark energy equation of state parameter $w$, DESI BAO alone require $w=-0.99^{+0.15}_{-0.13}$. In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with CMB or with SN~Ia individually prefer $w_0>-1$ and $w_a<0$. This preference is 2.6$蟽$ for the DESI+CMB combination, and persists or grows when SN~Ia are added in, giving results discrepant with the $螞$CDM model at the $2.5蟽$, $3.5蟽$ or $3.9蟽$ levels for the addition of Pantheon+, Union3, or DES-SN5YR datasets respectively. For the flat $螞$CDM model with the sum of neutrino mass $\sum m_谓$ free, combining the DESI and CMB data yields an upper limit $\sum m_谓< 0.072$ $(0.113)$ eV at 95% confidence for a $\sum m_谓>0$ $(\sum m_谓>0.059)$ eV prior. These neutrino-mass constraints are substantially relaxed in models beyond $螞$CDM. [Abridged.] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03002v3-abstract-full').style.display = 'none'; document.getElementById('2404.03002v3-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> 4 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers). 68 pages, 15 figures. Version accepted for publication in JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03001">arXiv:2404.03001</a> <span> [<a href="https://arxiv.org/pdf/2404.03001">pdf</a>, <a href="https://arxiv.org/format/2404.03001">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.1088/1475-7516/2025/01/124">10.1088/1475-7516/2025/01/124 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> DESI 2024 IV: Baryon Acoustic Oscillations from the Lyman Alpha Forest </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a> , et al. (174 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="2404.03001v4-abstract-short" style="display: inline;"> We present the measurement of Baryon Acoustic Oscillations (BAO) from the Lyman-$伪$ (Ly$伪$) forest of high-redshift quasars with the first-year dataset of the Dark Energy Spectroscopic Instrument (DESI). Our analysis uses over $420\,000$ Ly$伪$ forest spectra and their correlation with the spatial distribution of more than $700\,000$ quasars. An essential facet of this work is the development of a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03001v4-abstract-full').style.display = 'inline'; document.getElementById('2404.03001v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03001v4-abstract-full" style="display: none;"> We present the measurement of Baryon Acoustic Oscillations (BAO) from the Lyman-$伪$ (Ly$伪$) forest of high-redshift quasars with the first-year dataset of the Dark Energy Spectroscopic Instrument (DESI). Our analysis uses over $420\,000$ Ly$伪$ forest spectra and their correlation with the spatial distribution of more than $700\,000$ quasars. An essential facet of this work is the development of a new analysis methodology on a blinded dataset. We conducted rigorous tests using synthetic data to ensure the reliability of our methodology and findings before unblinding. Additionally, we conducted multiple data splits to assess the consistency of the results and scrutinized various analysis approaches to confirm their robustness. For a given value of the sound horizon ($r_d$), we measure the expansion at $z_{\rm eff}=2.33$ with 2\% precision, $H(z_{\rm eff}) = (239.2 \pm 4.8) (147.09~{\rm Mpc} /r_d)$ km/s/Mpc. Similarly, we present a 2.4\% measurement of the transverse comoving distance to the same redshift, $D_M(z_{\rm eff}) = (5.84 \pm 0.14) (r_d/147.09~{\rm Mpc})$ Gpc. Together with other DESI BAO measurements at lower redshifts, these results are used in a companion paper to constrain cosmological parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03001v4-abstract-full').style.display = 'none'; document.getElementById('2404.03001v4-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers). Minor changes in v4, version accepted for publication in JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03000">arXiv:2404.03000</a> <span> [<a href="https://arxiv.org/pdf/2404.03000">pdf</a>, <a href="https://arxiv.org/format/2404.03000">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">H. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">F. Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">C. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brieden%2C+S">S. Brieden</a>, <a href="/search/astro-ph?searchtype=author&query=Brodzeller%2C+A">A. Brodzeller</a> , et al. (171 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="2404.03000v1-abstract-short" style="display: inline;"> We present the DESI 2024 galaxy and quasar baryon acoustic oscillations (BAO) measurements using over 5.7 million unique galaxy and quasar redshifts in the range 0.1<z<2.1. Divided by tracer type, we utilize 300,017 galaxies from the magnitude-limited Bright Galaxy Survey with 0.1<z<0.4, 2,138,600 Luminous Red Galaxies with 0.4<z<1.1, 2,432,022 Emission Line Galaxies with 0.8<z<1.6, and 856,652 qu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03000v1-abstract-full').style.display = 'inline'; document.getElementById('2404.03000v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03000v1-abstract-full" style="display: none;"> We present the DESI 2024 galaxy and quasar baryon acoustic oscillations (BAO) measurements using over 5.7 million unique galaxy and quasar redshifts in the range 0.1<z<2.1. Divided by tracer type, we utilize 300,017 galaxies from the magnitude-limited Bright Galaxy Survey with 0.1<z<0.4, 2,138,600 Luminous Red Galaxies with 0.4<z<1.1, 2,432,022 Emission Line Galaxies with 0.8<z<1.6, and 856,652 quasars with 0.8<z<2.1, over a ~7,500 square degree footprint. The analysis was blinded at the catalog-level to avoid confirmation bias. All fiducial choices of the BAO fitting and reconstruction methodology, as well as the size of the systematic errors, were determined on the basis of the tests with mock catalogs and the blinded data catalogs. We present several improvements to the BAO analysis pipeline, including enhancing the BAO fitting and reconstruction methods in a more physically-motivated direction, and also present results using combinations of tracers. We present a re-analysis of SDSS BOSS and eBOSS results applying the improved DESI methodology and find scatter consistent with the level of the quoted SDSS theoretical systematic uncertainties. With the total effective survey volume of ~ 18 Gpc$^3$, the combined precision of the BAO measurements across the six different redshift bins is ~0.52%, marking a 1.2-fold improvement over the previous state-of-the-art results using only first-year data. We detect the BAO in all of these six redshift bins. The highest significance of BAO detection is $9.1蟽$ at the effective redshift of 0.93, with a constraint of 0.86% placed on the BAO scale. We find our measurements are systematically larger than the prediction of Planck-2018 LCDM model at z<0.8. We translate the results into transverse comoving distance and radial Hubble distance measurements, which are used to constrain cosmological models in our companion paper [abridged]. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03000v1-abstract-full').style.display = 'none'; document.getElementById('2404.03000v1-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 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">This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.18789">arXiv:2403.18789</a> <span> [<a href="https://arxiv.org/pdf/2403.18789">pdf</a>, <a href="https://arxiv.org/format/2403.18789">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Constraining primordial non-Gaussianity from the large scale structure two-point and three-point correlation functions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brown%2C+Z">Z. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Demina%2C+R">R. Demina</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Chaussidon%2C+E">E. Chaussidon</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+S">S. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez-Perez%2C+V">V. Gonzalez-Perez</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Bellido%2C+J">J. Garc铆a-Bellido</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">B. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">K. Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">S. Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">R. Kehoe</a> , et al. (25 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="2403.18789v1-abstract-short" style="display: inline;"> Surveys of cosmological large-scale structure (LSS) are sensitive to the presence of local primordial non-Gaussianity (PNG), and may be used to constrain models of inflation. Local PNG, characterized by fNL, the amplitude of the quadratic correction to the potential of a Gaussian random field, is traditionally measured from LSS two-point and three-point clustering via the power spectrum and bi-spe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18789v1-abstract-full').style.display = 'inline'; document.getElementById('2403.18789v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.18789v1-abstract-full" style="display: none;"> Surveys of cosmological large-scale structure (LSS) are sensitive to the presence of local primordial non-Gaussianity (PNG), and may be used to constrain models of inflation. Local PNG, characterized by fNL, the amplitude of the quadratic correction to the potential of a Gaussian random field, is traditionally measured from LSS two-point and three-point clustering via the power spectrum and bi-spectrum. We propose a framework to measure fNL using the configuration space two-point correlation function (2pcf) monopole and three-point correlation function (3pcf) monopole of survey tracers. Our model estimates the effect of the scale-dependent bias induced by the presence of PNG on the 2pcf and 3pcf from the clustering of simulated dark matter halos. We describe how this effect may be scaled to an arbitrary tracer of the cosmological matter density. The 2pcf and 3pcf of this tracer are measured to constrain the value of fNL. Using simulations of luminous red galaxies observed by the Dark Energy Spectroscopic Instrument (DESI), we demonstrate the accuracy and constraining power of our model, and forecast the ability to constrainfNL to a precision of sigma(fNL) = 22 with one year of DESI survey data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18789v1-abstract-full').style.display = 'none'; document.getElementById('2403.18789v1-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.18644">arXiv:2402.18644</a> <span> [<a href="https://arxiv.org/pdf/2402.18644">pdf</a>, <a href="https://arxiv.org/format/2402.18644">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The frequency of metal-enrichment of cool helium-atmosphere white dwarfs using the DESI Early Data Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Manser%2C+C+J">Christopher J. Manser</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=Izquierdo%2C+P">Paula Izquierdo</a>, <a href="/search/astro-ph?searchtype=author&query=Swan%2C+A">Andrew Swan</a>, <a href="/search/astro-ph?searchtype=author&query=Najita%2C+J">Joan Najita</a>, <a href="/search/astro-ph?searchtype=author&query=Rockosi%2C+C">C. Rockosi</a>, <a href="/search/astro-ph?searchtype=author&query=Carrillo%2C+A">Andreia Carrillo</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+B">Bokyoung Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+S">Siyi Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">R. Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Kremin%2C+A">A. Kremin</a>, <a href="/search/astro-ph?searchtype=author&query=Landriau%2C+M">M. Landriau</a>, <a href="/search/astro-ph?searchtype=author&query=Guillou%2C+L+L">L. Le Guillou</a> , et al. (13 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="2402.18644v1-abstract-short" style="display: inline;"> There is overwhelming evidence that white dwarfs host planetary systems; revealed by the presence, disruption, and accretion of planetary bodies. A lower limit on the frequency of white dwarfs that host planetary material has been estimated to be roughly 25-50 per cent; inferred from the ongoing or recent accretion of metals onto both hydrogen-atmosphere and warm helium-atmosphere white dwarfs. No… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18644v1-abstract-full').style.display = 'inline'; document.getElementById('2402.18644v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.18644v1-abstract-full" style="display: none;"> There is overwhelming evidence that white dwarfs host planetary systems; revealed by the presence, disruption, and accretion of planetary bodies. A lower limit on the frequency of white dwarfs that host planetary material has been estimated to be roughly 25-50 per cent; inferred from the ongoing or recent accretion of metals onto both hydrogen-atmosphere and warm helium-atmosphere white dwarfs. Now with the unbiased sample of white dwarfs observed by the Dark Energy Spectroscopic Instrument (DESI) survey in their Early Data Release (EDR), we have determined the frequency of metal-enrichment around cool-helium atmosphere white dwarfs as 21 $\pm$ 3 per cent using a sample of 234 systems. This value is in good agreement with values determined from previous studies. With the current samples we cannot distinguish whether the frequency of planetary accretion varies with system age or host-star mass, but the DESI data release 1 will contain roughly an order of magnitude more white dwarfs than DESI EDR and will allow these parameters to be investigated. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18644v1-abstract-full').style.display = 'none'; document.getElementById('2402.18644v1-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">6 pages, 1 figure. Submitted to MNRAS. Comments and suggestions welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.18641">arXiv:2402.18641</a> <span> [<a href="https://arxiv.org/pdf/2402.18641">pdf</a>, <a href="https://arxiv.org/format/2402.18641">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> <span class="tag is-small is-grey 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> <p class="title is-5 mathjax"> The DESI Early Data Release White Dwarf Catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Manser%2C+C+J">Christopher J. Manser</a>, <a href="/search/astro-ph?searchtype=author&query=Izquierdo%2C+P">Paula Izquierdo</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=Swan%2C+A">Andrew Swan</a>, <a href="/search/astro-ph?searchtype=author&query=Koester%2C+D">Detlev Koester</a>, <a href="/search/astro-ph?searchtype=author&query=Robert%2C+A">Akshay Robert</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+S">Siyi Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Inight%2C+K">Keith Inight</a>, <a href="/search/astro-ph?searchtype=author&query=Amroota%2C+B">Ben Amroota</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=Koposov%2C+S+E">Sergey E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+B">Bokyoung Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</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=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+A+P">A. P. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a> , et al. (29 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="2402.18641v1-abstract-short" style="display: inline;"> The Early Data Release (EDR) of the Dark Energy Spectroscopic Instrument (DESI) comprises spectroscopy obtained from 2020 December 14 to 2021 June 10. White dwarfs were targeted by DESI both as calibration sources and as science targets and were selected based on Gaia photometry and astrometry. Here we present the DESI EDR white dwarf catalogue, which includes 2706 spectroscopically confirmed whit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18641v1-abstract-full').style.display = 'inline'; document.getElementById('2402.18641v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.18641v1-abstract-full" style="display: none;"> The Early Data Release (EDR) of the Dark Energy Spectroscopic Instrument (DESI) comprises spectroscopy obtained from 2020 December 14 to 2021 June 10. White dwarfs were targeted by DESI both as calibration sources and as science targets and were selected based on Gaia photometry and astrometry. Here we present the DESI EDR white dwarf catalogue, which includes 2706 spectroscopically confirmed white dwarfs of which approximately 1630 (roughly 60 per cent) have been spectroscopically observed for the first time, as well as 66 white dwarf binary systems. We provide spectral classifications for all white dwarfs, and discuss their distribution within the Gaia Hertzsprung-Russell diagram. We provide atmospheric parameters derived from spectroscopic and photometric fits for white dwarfs with pure hydrogen or helium photospheres, a mixture of those two, and white dwarfs displaying carbon features in their spectra. We also discuss the less abundant systems in the sample, such as those with magnetic fields, and cataclysmic variables. The DESI EDR white dwarf sample is significantly less biased than the sample observed by the Sloan Digital Sky Survey, which is skewed to bluer and therefore hotter white dwarfs, making DESI more complete and suitable for performing statistical studies of white dwarfs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18641v1-abstract-full').style.display = 'none'; document.getElementById('2402.18641v1-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">19 pages, 17 figures, not including appendix. Submitting to MNRAS. Comments and suggestions welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.14070">arXiv:2402.14070</a> <span> [<a href="https://arxiv.org/pdf/2402.14070">pdf</a>, <a href="https://arxiv.org/format/2402.14070">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Baryon Acoustic Oscillation Theory and Modelling Systematics for the DESI 2024 results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">Shi-Fan Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">Cullan Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+M">Martin White</a>, <a href="/search/astro-ph?searchtype=author&query=McDonald%2C+P">Patrick McDonald</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=Seo%2C+H">Hee-Jong Seo</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabhan%2C+N">Nikhil Padmanabhan</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+U">U. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">S. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Z">Z. Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-S%C3%A1nchez%2C+D">D. Forero-S谩nchez</a> , et al. (36 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="2402.14070v2-abstract-short" style="display: inline;"> This paper provides a comprehensive overview of how fitting of Baryon Acoustic Oscillations (BAO) is carried out within the upcoming Dark Energy Spectroscopic Instrument's (DESI) 2024 results using its DR1 dataset, and the associated systematic error budget from theory and modelling of the BAO. We derive new results showing how non-linearities in the clustering of galaxies can cause potential bias… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.14070v2-abstract-full').style.display = 'inline'; document.getElementById('2402.14070v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.14070v2-abstract-full" style="display: none;"> This paper provides a comprehensive overview of how fitting of Baryon Acoustic Oscillations (BAO) is carried out within the upcoming Dark Energy Spectroscopic Instrument's (DESI) 2024 results using its DR1 dataset, and the associated systematic error budget from theory and modelling of the BAO. We derive new results showing how non-linearities in the clustering of galaxies can cause potential biases in measurements of the isotropic ($伪_{\mathrm{iso}}$) and anisotropic ($伪_{\mathrm{ap}}$) BAO distance scales, and how these can be effectively removed with an appropriate choice of reconstruction algorithm. We then demonstrate how theory leads to a clear choice for how to model the BAO and develop, implement and validate a new model for the remaining smooth-broadband (i.e., without BAO) component of the galaxy clustering. Finally, we explore the impact of all remaining modelling choices on the BAO constraints from DESI using a suite of high-precision simulations, arriving at a set of best-practices for DESI BAO fits, and an associated theory and modelling systematic error. Overall, our results demonstrate the remarkable robustness of the BAO to all our modelling choices and motivate a combined theory and modelling systematic error contribution to the post-reconstruction DESI BAO measurements of no more than $0.1\%$ ($0.2\%$) for its isotropic (anisotropic) distance measurements. We expect the theory and best-practices laid out to here to be applicable to other BAO experiments in the era of DESI and beyond. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.14070v2-abstract-full').style.display = 'none'; document.getElementById('2402.14070v2-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> 4 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">30 pages, 18 figures, 1 table, updated to match version 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/2402.02378">arXiv:2402.02378</a> <span> [<a href="https://arxiv.org/pdf/2402.02378">pdf</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> <p class="title is-5 mathjax"> Maximizing the scientific return of Roman and Rubin with a joint wide-sky observing strategy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">Federica B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+A">Andrew Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+M">Melissa Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+L">Leanne Guy</a>, <a href="/search/astro-ph?searchtype=author&query=Ivezic%2C+Z">Zeljko Ivezic</a>, <a href="/search/astro-ph?searchtype=author&query=Ritz%2C+S">Steve Ritz</a>, <a href="/search/astro-ph?searchtype=author&query=Strauss%2C+M+A">Michael A. Strauss</a>, <a href="/search/astro-ph?searchtype=author&query=Tyson%2C+T">Tony Tyson</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="2402.02378v1-abstract-short" style="display: inline;"> This work presents the case for a single-band LSST-matched depth Roman Community Survey over the footprint of the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) Wide-Fast-Deep to enhance the key science programs of both missions. We propose to observe the ~18K sq deg LSST Wide-Fast-Deep footprint in the F146 filter to mAB~25; this will take approximately 5 months of Roman observi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.02378v1-abstract-full').style.display = 'inline'; document.getElementById('2402.02378v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.02378v1-abstract-full" style="display: none;"> This work presents the case for a single-band LSST-matched depth Roman Community Survey over the footprint of the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) Wide-Fast-Deep to enhance the key science programs of both missions. We propose to observe the ~18K sq deg LSST Wide-Fast-Deep footprint in the F146 filter to mAB~25; this will take approximately 5 months of Roman observing time. The combination of the multiwavelength nature of LSST and angular resolution of Roman would lead to enhanced scientific returns for both the Roman and LSST surveys. Galaxy deblending and crowded field photometry will be significantly improved. The extension of Rubin LSST six-band optical photometry to IR wavelengths would improve photometric redshift (photo-z) estimation, leading to improved cosmological parameter estimation, penetrate interstellar dust in the Galactic plane, improve differential chromatic refraction derived Spectral Energy Distributions, maximize galaxy-star separation and minimize crowding confusion through improved angular resolution. Conversely, the LSST survey will provide a time-domain extension of the Roman survey on the shared footprint and 6-band optical photometry with sensitivity extending all the way to ultraviolet wavelengths. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.02378v1-abstract-full').style.display = 'none'; document.getElementById('2402.02378v1-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> 4 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">This document was written in response to the Call for Community Input into the Definition of the Roman Space Telescope's Core Community Surveys (June 2023)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.13062">arXiv:2311.13062</a> <span> [<a href="https://arxiv.org/pdf/2311.13062">pdf</a>, <a href="https://arxiv.org/format/2311.13062">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> A dark siren measurement of the Hubble constant with the LIGO/Virgo gravitational wave event GW190412 and DESI galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ballard%2C+W">W. Ballard</a>, <a href="/search/astro-ph?searchtype=author&query=Palmese%2C+A">A. Palmese</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez%2C+I+M">I. Maga帽a Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Moon%2C+J">J. Moon</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</a>, <a href="/search/astro-ph?searchtype=author&query=Rossi%2C+G">G. Rossi</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">A. de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">A. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">S. Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Kremin%2C+A">A. Kremin</a>, <a href="/search/astro-ph?searchtype=author&query=Manera%2C+M">M. Manera</a>, <a href="/search/astro-ph?searchtype=author&query=Meisner%2C+A">A. Meisner</a>, <a href="/search/astro-ph?searchtype=author&query=Miquel%2C+R">R. Miquel</a>, <a href="/search/astro-ph?searchtype=author&query=Moustakas%2C+J">J. Moustakas</a>, <a href="/search/astro-ph?searchtype=author&query=Prada%2C+F">F. Prada</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+E">E. Sanchez</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="2311.13062v1-abstract-short" style="display: inline;"> We present a measurement of the Hubble Constant $H_0$ using the gravitational wave event GW190412, an asymmetric binary black hole merger detected by LIGO/Virgo, as a dark standard siren. This event does not have an electromagnetic counterpart, so we use the statistical standard siren method and marginalize over potential host galaxies from the Dark Energy Spectroscopic Instrument (DESI) survey. G… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13062v1-abstract-full').style.display = 'inline'; document.getElementById('2311.13062v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.13062v1-abstract-full" style="display: none;"> We present a measurement of the Hubble Constant $H_0$ using the gravitational wave event GW190412, an asymmetric binary black hole merger detected by LIGO/Virgo, as a dark standard siren. This event does not have an electromagnetic counterpart, so we use the statistical standard siren method and marginalize over potential host galaxies from the Dark Energy Spectroscopic Instrument (DESI) survey. GW190412 is well-localized to 12 deg$^2$ (90% credible interval), so it is promising for a dark siren analysis. The dark siren value for $H_0=85.4_{-33.9}^{+29.1}$ km/s/Mpc, with a posterior shape that is consistent with redshift overdensities. When combined with the bright standard siren measurement from GW170817 we recover $H_0=77.96_{-5.03}^{+23.0}$ km/s/Mpc, consistent with both early and late-time Universe measurements of $H_0$. This work represents the first standard siren analysis performed with DESI data, and includes the most complete spectroscopic sample used in a dark siren analysis to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13062v1-abstract-full').style.display = 'none'; document.getElementById('2311.13062v1-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 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">Submitted to RNAAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.12177">arXiv:2310.12177</a> <span> [<a href="https://arxiv.org/pdf/2310.12177">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Physics and Society">physics.soc-ph</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> <p class="title is-5 mathjax"> Anti-Black racism workshop during the Vera C. Rubin Observatory virtual 2021 Project and Community Workshop </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Malag%C3%B3n%2C+A+A+P">Andr茅s A. Plazas Malag贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F">Federica Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+R">Ranpal Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Rosaria"> Rosaria</a>, <a href="/search/astro-ph?searchtype=author&query=Bonito"> Bonito</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Mullane%2C+W">Wil O'Mullane</a>, <a href="/search/astro-ph?searchtype=author&query=Shugart%2C+A">Alsyha Shugart</a>, <a href="/search/astro-ph?searchtype=author&query=Street%2C+R">Rachel Street</a>, <a href="/search/astro-ph?searchtype=author&query=Verma%2C+A">Aprajita Verma</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="2310.12177v1-abstract-short" style="display: inline;"> Systemic racism is a ubiquitous theme in societies worldwide and plays a central role in shaping our economic, social, and academic institutions. The Vera C. Rubin Observatory is a major US ground-based facility based in Chile with international participation. The Observatory is an example of excellence and will deliver the largest survey of the sky ever attempted. Rubin's full scientific and soci… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.12177v1-abstract-full').style.display = 'inline'; document.getElementById('2310.12177v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.12177v1-abstract-full" style="display: none;"> Systemic racism is a ubiquitous theme in societies worldwide and plays a central role in shaping our economic, social, and academic institutions. The Vera C. Rubin Observatory is a major US ground-based facility based in Chile with international participation. The Observatory is an example of excellence and will deliver the largest survey of the sky ever attempted. Rubin's full scientific and social potential can not be attained without addressing systemic racism and associated barriers to equity, diversity, and inclusion (EDI). During Rubin's 2021 virtual Project and Community Workshop (PCW), the annual Rubin community-based meeting, an anti-Black racism workshop took place, facilitated by 'The BIPOC Project' organization. About 60 members from different parts of the Rubin ecosystem participated. We describe the motivation, organization, challenges, outcomes, and near- and long-term goals of this workshop. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.12177v1-abstract-full').style.display = 'none'; document.getElementById('2310.12177v1-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> 16 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Contribution to appear in 'An Astronomical Inclusion Revolution: Advancing Diversity, Equity, and Inclusion in Professional Astronomy and Astrophysics', to be published by IOP ebooks</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.13609">arXiv:2306.13609</a> <span> [<a href="https://arxiv.org/pdf/2306.13609">pdf</a>, <a href="https://arxiv.org/format/2306.13609">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Optics">physics.optics</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/10.1038/s41467-024-51560-x">10.1038/s41467-024-51560-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ultraviolet astronomical spectrograph calibration with laser frequency combs from nanophotonic lithium niobate waveguides </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ludwig%2C+M">Markus Ludwig</a>, <a href="/search/astro-ph?searchtype=author&query=Ayhan%2C+F">Furkan Ayhan</a>, <a href="/search/astro-ph?searchtype=author&query=Schmidt%2C+T+M">Tobias M. Schmidt</a>, <a href="/search/astro-ph?searchtype=author&query=Wildi%2C+T">Thibault Wildi</a>, <a href="/search/astro-ph?searchtype=author&query=Voumard%2C+T">Thibault Voumard</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Roman Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Ye%2C+Z">Zhichao Ye</a>, <a href="/search/astro-ph?searchtype=author&query=Lei%2C+F">Fuchuan Lei</a>, <a href="/search/astro-ph?searchtype=author&query=Wildi%2C+F">Fran莽ois Wildi</a>, <a href="/search/astro-ph?searchtype=author&query=Pepe%2C+F">Francesco Pepe</a>, <a href="/search/astro-ph?searchtype=author&query=Gaafar%2C+M+A">Mahmoud A. Gaafar</a>, <a href="/search/astro-ph?searchtype=author&query=Obrzud%2C+E">Ewelina Obrzud</a>, <a href="/search/astro-ph?searchtype=author&query=Grassani%2C+D">Davide Grassani</a>, <a href="/search/astro-ph?searchtype=author&query=Hefti%2C+O">Olivia Hefti</a>, <a href="/search/astro-ph?searchtype=author&query=Karlen%2C+S">Sylvain Karlen</a>, <a href="/search/astro-ph?searchtype=author&query=Lecomte%2C+S">Steve Lecomte</a>, <a href="/search/astro-ph?searchtype=author&query=Moreau%2C+F">Fran莽ois Moreau</a>, <a href="/search/astro-ph?searchtype=author&query=Chazelas%2C+B">Bruno Chazelas</a>, <a href="/search/astro-ph?searchtype=author&query=Sottile%2C+R">Rico Sottile</a>, <a href="/search/astro-ph?searchtype=author&query=Torres-Company%2C+V">Victor Torres-Company</a>, <a href="/search/astro-ph?searchtype=author&query=Brasch%2C+V">Victor Brasch</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+L+G">Luis G. Villanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchy%2C+F">Fran莽ois Bouchy</a>, <a href="/search/astro-ph?searchtype=author&query=Herr%2C+T">Tobias Herr</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="2306.13609v2-abstract-short" style="display: inline;"> Astronomical precision spectroscopy underpins searches for life beyond Earth, direct observation of the expanding Universe and constraining the potential variability of physical constants across cosmological scales. Laser frequency combs can provide the critically required accurate and precise calibration to the astronomical spectrographs. For cosmological studies, extending the calibration with s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.13609v2-abstract-full').style.display = 'inline'; document.getElementById('2306.13609v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.13609v2-abstract-full" style="display: none;"> Astronomical precision spectroscopy underpins searches for life beyond Earth, direct observation of the expanding Universe and constraining the potential variability of physical constants across cosmological scales. Laser frequency combs can provide the critically required accurate and precise calibration to the astronomical spectrographs. For cosmological studies, extending the calibration with such astrocombs to the ultraviolet spectral range is highly desirable, however, strong material dispersion and large spectral separation from the established infrared laser oscillators have made this exceedingly challenging. Here, we demonstrate for the first time astronomical spectrograph calibrations with an astrocomb in the ultraviolet spectral range below 400 nm. This is accomplished via chip-integrated highly nonlinear photonics in periodically-poled, nano-fabricated lithium niobate waveguides in conjunction with a robust infrared electro-optic comb generator, as well as a chip-integrated microresonator comb. These results demonstrate a viable route towards astronomical precision spectroscopy in the ultraviolet and may contribute to unlocking the full potential of next generation ground- and future space-based astronomical instruments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.13609v2-abstract-full').style.display = 'none'; document.getElementById('2306.13609v2-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> 17 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">Journal ref:</span> Nat Commun 15, 7614 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.06308">arXiv:2306.06308</a> <span> [<a href="https://arxiv.org/pdf/2306.06308">pdf</a>, <a href="https://arxiv.org/format/2306.06308">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/ad3217">10.3847/1538-3881/ad3217 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Early Data Release of the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Aldering%2C+G">G. Aldering</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alfarsy%2C+R">R. Alfarsy</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Balaguera-Antol%C3%ADnez%2C+A">A. Balaguera-Antol铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">O. Ballester</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=Beltran%2C+S+F">S. F. Beltran</a> , et al. (244 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="2306.06308v3-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) completed its five-month Survey Validation in May 2021. Spectra of stellar and extragalactic targets from Survey Validation constitute the first major data sample from the DESI survey. This paper describes the public release of those spectra, the catalogs of derived properties, and the intermediate data products. In total, the public release includes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06308v3-abstract-full').style.display = 'inline'; document.getElementById('2306.06308v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06308v3-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) completed its five-month Survey Validation in May 2021. Spectra of stellar and extragalactic targets from Survey Validation constitute the first major data sample from the DESI survey. This paper describes the public release of those spectra, the catalogs of derived properties, and the intermediate data products. In total, the public release includes good-quality spectral information from 466,447 objects targeted as part of the Milky Way Survey, 428,758 as part of the Bright Galaxy Survey, 227,318 as part of the Luminous Red Galaxy sample, 437,664 as part of the Emission Line Galaxy sample, and 76,079 as part of the Quasar sample. In addition, the release includes spectral information from 137,148 objects that expand the scope beyond the primary samples as part of a series of secondary programs. Here, we describe the spectral data, data quality, data products, Large-Scale Structure science catalogs, access to the data, and references that provide relevant background to using these spectra. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06308v3-abstract-full').style.display = 'none'; document.getElementById('2306.06308v3-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> 17 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 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">43 pages, 7 figures, 17 tables, accepted for publication in the Astronomical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> AJ 168 58 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.06307">arXiv:2306.06307</a> <span> [<a href="https://arxiv.org/pdf/2306.06307">pdf</a>, <a href="https://arxiv.org/format/2306.06307">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.5281/zenodo.7858207">10.5281/zenodo.7858207 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adame%2C+A+G">A. G. Adame</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">S. Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Aldering%2C+G">G. Aldering</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alfarsy%2C+R">R. Alfarsy</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">M. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">A. Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Balaguera-Antol%C3%ADnez%2C+A">A. Balaguera-Antol铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">O. Ballester</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+J">J. Bautista</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">J. Behera</a>, <a href="/search/astro-ph?searchtype=author&query=Beltran%2C+S+F">S. F. Beltran</a> , et al. (239 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="2306.06307v3-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg$^2$ over five years to constrain the cosmic expansion history through precise measurements of Baryon Acoustic Oscillations (BAO). The scientific program for DESI was evaluated during a five month Survey Validation (SV) campaign before beginning full operations. This program produced deep spectra of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06307v3-abstract-full').style.display = 'inline'; document.getElementById('2306.06307v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06307v3-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg$^2$ over five years to constrain the cosmic expansion history through precise measurements of Baryon Acoustic Oscillations (BAO). The scientific program for DESI was evaluated during a five month Survey Validation (SV) campaign before beginning full operations. This program produced deep spectra of tens of thousands of objects from each of the stellar (MWS), bright galaxy (BGS), luminous red galaxy (LRG), emission line galaxy (ELG), and quasar target classes. These SV spectra were used to optimize redshift distributions, characterize exposure times, determine calibration procedures, and assess observational overheads for the five-year program. In this paper, we present the final target selection algorithms, redshift distributions, and projected cosmology constraints resulting from those studies. We also present a `One-Percent survey' conducted at the conclusion of Survey Validation covering 140 deg$^2$ using the final target selection algorithms with exposures of a depth typical of the main survey. The Survey Validation indicates that DESI will be able to complete the full 14,000 deg$^2$ program with spectroscopically-confirmed targets from the MWS, BGS, LRG, ELG, and quasar programs with total sample sizes of 7.2, 13.8, 7.46, 15.7, and 2.87 million, respectively. These samples will allow exploration of the Milky Way halo, clustering on all scales, and BAO measurements with a statistical precision of 0.28% over the redshift interval $z<1.1$, 0.39% over the redshift interval $1.1<z<1.9$, and 0.46% over the redshift interval $1.9<z<3.5$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06307v3-abstract-full').style.display = 'none'; document.getElementById('2306.06307v3-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 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">42 pages, 18 figures, accepted 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/2304.08427">arXiv:2304.08427</a> <span> [<a href="https://arxiv.org/pdf/2304.08427">pdf</a>, <a href="https://arxiv.org/format/2304.08427">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/stad2618">10.1093/mnras/stad2618 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </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/stad2618">10.1093/mnras/stad2618 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Detection of the BAO Signal from Early DESI Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Moon%2C+J">Jeongin Moon</a>, <a href="/search/astro-ph?searchtype=author&query=Valcin%2C+D">David Valcin</a>, <a href="/search/astro-ph?searchtype=author&query=Rashkovetskyi%2C+M">Michael Rashkovetskyi</a>, <a href="/search/astro-ph?searchtype=author&query=Saulder%2C+C">Christoph Saulder</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">Jessica Nicole Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">Shadab Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">Stephen Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">Charles Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">Etienne Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Chaussidon%2C+E">Edmond Chaussidon</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">Kyle Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mattia%2C+A">Arnaud de Mattia</a>, <a href="/search/astro-ph?searchtype=author&query=Dhungana%2C+G">Govinda Dhungana</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenstein%2C+D">Daniel Eisenstein</a>, <a href="/search/astro-ph?searchtype=author&query=Flaugher%2C+B">Brenna Flaugher</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Quintero%2C+C">Cristhian Garcia-Quintero</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">Satya Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+J">Julien Guy</a>, <a href="/search/astro-ph?searchtype=author&query=Hanif%2C+M+M+S">Malik Muhammad Sikandar Hanif</a> , et al. (43 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="2304.08427v2-abstract-short" style="display: inline;"> We present the first detection of the baryon acoustic oscillations (BAO) signal obtained using unblinded data collected during the initial two months of operations of the Stage-IV ground-based Dark Energy Spectroscopic Instrument (DESI). From a selected sample of 261,291 Luminous Red Galaxies spanning the redshift interval 0.4 < z < 1.1 and covering 1651 square degrees with a 57.9% completeness le… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.08427v2-abstract-full').style.display = 'inline'; document.getElementById('2304.08427v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.08427v2-abstract-full" style="display: none;"> We present the first detection of the baryon acoustic oscillations (BAO) signal obtained using unblinded data collected during the initial two months of operations of the Stage-IV ground-based Dark Energy Spectroscopic Instrument (DESI). From a selected sample of 261,291 Luminous Red Galaxies spanning the redshift interval 0.4 < z < 1.1 and covering 1651 square degrees with a 57.9% completeness level, we report a ~5 sigma level BAO detection and the measurement of the BAO location at a precision of 1.7%. Using a Bright Galaxy Sample of 109,523 galaxies in the redshift range 0.1 < z < 0.5, over 3677 square degrees with a 50.0% completeness, we also detect the BAO feature at ~3 sigma significance with a 2.6% precision. These first BAO measurements represent an important milestone, acting as a quality control on the optimal performance of the complex robotically-actuated, fiber-fed DESI spectrograph, as well as an early validation of the DESI spectroscopic pipeline and data management system. Based on these first promising results, we forecast that DESI is on target to achieve a high-significance BAO detection at sub-percent precision with the completed 5-year survey data, meeting the top-level science requirements on BAO measurements. This exquisite level of precision will set new standards in cosmology and confirm DESI as the most competitive BAO experiment for the remainder of this decade. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.08427v2-abstract-full').style.display = 'none'; document.getElementById('2304.08427v2-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">17 pages, 10 figures, 4 tables. MNRAS, 525, 5406. Author accepted manuscript matching the published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Monthly Notices of the Royal Astronomical Society, Volume 525, Issue 4, November 2023, Pages 5406-5422 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.13841">arXiv:2211.13841</a> <span> [<a href="https://arxiv.org/pdf/2211.13841">pdf</a>, <a href="https://arxiv.org/ps/2211.13841">ps</a>, <a href="https://arxiv.org/format/2211.13841">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/aca079">10.3847/1538-4357/aca079 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Near-Infrared Spectroscopy of Ultracompact \ion{H}{2} regions in W51A with NIFS/ALTAIR </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barbosa%2C+C+L">Cassio L. Barbosa</a>, <a href="/search/astro-ph?searchtype=author&query=Navarete%2C+F">Felipe Navarete</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Damineli%2C+A">Augusto Damineli</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="2211.13841v1-abstract-short" style="display: inline;"> W51A is the most active star formation region of the Giant \ion{H}{2} region W51. It harbors the two massive proto-clusters W51e and W51\,IRS2, which are very rare in the Galaxy. We aim to identify the new born massive stars and UCHII regions to derive its distance and age. We performed IFU observations with NIFS+ALTAIR of nine targets in the W51A sub-region. The distance modulus was obtained usin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.13841v1-abstract-full').style.display = 'inline'; document.getElementById('2211.13841v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.13841v1-abstract-full" style="display: none;"> W51A is the most active star formation region of the Giant \ion{H}{2} region W51. It harbors the two massive proto-clusters W51e and W51\,IRS2, which are very rare in the Galaxy. We aim to identify the new born massive stars and UCHII regions to derive its distance and age. We performed IFU observations with NIFS+ALTAIR of nine targets in the W51A sub-region. The distance modulus was obtained using the spectral classification in the $K$-band and a reddening law appropriate to the inner Galactic plane. We derived the distance and the spectral types for five of them, ranging from O8 to O9.5, similar to those derived from radio continuum data, except for two sources that we assigned somewhat a later spectral type. We included another seven objects with precise spectral classification from other works, which allowed us to better constrain the distance estimate. Our spectrophotometric distance d=4.80\,$\pm$\,1.27\,kpc is in good agreement with those derived from the Galactic rotation model and trigonometric parallaxes, placing the region near the tangent point of the Sagittarius arm. We conclude that the stars studied in this work have an age spread of 1.5-4 Myr, substantially older than thought to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.13841v1-abstract-full').style.display = 'none'; document.getElementById('2211.13841v1-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 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">18 pages, 12 figures and 3 tables. Accepted to ApJ for publication</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.10939">arXiv:2205.10939</a> <span> [<a href="https://arxiv.org/pdf/2205.10939">pdf</a>, <a href="https://arxiv.org/format/2205.10939">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/ac882b">10.3847/1538-3881/ac882b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abareshi%2C+B">B. Abareshi</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">S. Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">Shadab Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Alfarsy%2C+R">R. Alfarsy</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+L">L. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Ameel%2C+J">J. Ameel</a>, <a href="/search/astro-ph?searchtype=author&query=Armengaud%2C+E">E. Armengaud</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Aviles%2C+A">Alejandro Aviles</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Balaguera-Antol%C3%ADnez%2C+A">A. Balaguera-Antol铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">O. Ballester</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bault%2C+A">A. Bault</a>, <a href="/search/astro-ph?searchtype=author&query=Beltran%2C+S+F">S. F. Beltran</a>, <a href="/search/astro-ph?searchtype=author&query=Benavides%2C+B">B. Benavides</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Besuner%2C+R">R. Besuner</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">Florian Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">D. Bianchi</a> , et al. (242 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="2205.10939v1-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) has embarked on an ambitious five-year survey to explore the nature of dark energy with spectroscopy of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the Baryon Acoustic Oscillation method to measure distances from the nearby universe to z > 3.5, as well as measure the growth of structure and probe potential modifi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.10939v1-abstract-full').style.display = 'inline'; document.getElementById('2205.10939v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.10939v1-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) has embarked on an ambitious five-year survey to explore the nature of dark energy with spectroscopy of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the Baryon Acoustic Oscillation method to measure distances from the nearby universe to z > 3.5, as well as measure the growth of structure and probe potential modifications to general relativity. In this paper we describe the significant instrumentation we developed for the DESI survey. The new instrumentation includes a wide-field, 3.2-deg diameter prime-focus corrector that focuses the light onto 5020 robotic fiber positioners on the 0.812 m diameter, aspheric focal surface. The positioners and their fibers are divided among ten wedge-shaped petals. Each petal is connected to one of ten spectrographs via a contiguous, high-efficiency, nearly 50 m fiber cable bundle. The ten spectrographs each use a pair of dichroics to split the light into three channels that together record the light from 360 - 980 nm with a resolution of 2000 to 5000. We describe the science requirements, technical requirements on the instrumentation, and management of the project. DESI was installed at the 4-m Mayall telescope at Kitt Peak, and we also describe the facility upgrades to prepare for DESI and the installation and functional verification process. DESI has achieved all of its performance goals, and the DESI survey began in May 2021. Some performance highlights include RMS positioner accuracy better than 0.1", SNR per \sqrt脜 > 0.5 for a z > 2 quasar with flux 0.28e-17 erg/s/cm^2/A at 380 nm in 4000s, and median SNR = 7 of the [OII] doublet at 8e-17 erg/s/cm^2 in a 1000s exposure for emission line galaxies at z = 1.4 - 1.6. We conclude with highlights from the on-sky validation and commissioning of the instrument, key successes, and lessons learned. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.10939v1-abstract-full').style.display = 'none'; document.getElementById('2205.10939v1-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> 22 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">78 pages, 32 figures, submitted 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/2108.01683">arXiv:2108.01683</a> <span> [<a href="https://arxiv.org/pdf/2108.01683">pdf</a>, <a href="https://arxiv.org/format/2108.01683">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/10.3847/1538-4365/ac3e72">10.3847/1538-4365/ac3e72 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optimization of the Observing Cadence for the Rubin Observatory Legacy Survey of Space and Time: a pioneering process of community-focused experimental design </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">Federica B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Ivezi%C4%87%2C+%C5%BD">沤eljko Ivezi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+R+L">R. Lynne Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+M+L">Melissa L. Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+P">Phil Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Saha%2C+A">Abhijit Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Strauss%2C+M+A">Michael A. Strauss</a>, <a href="/search/astro-ph?searchtype=author&query=Yoachim%2C+P">Peter Yoachim</a>, <a href="/search/astro-ph?searchtype=author&query=Ribeiro%2C+T">Tiago Ribeiro</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+T">Timo Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Bellm%2C+E+C">Eric C. Bellm</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+W+N">William N. Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M脿rcio Catelan</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=Connolly%2C+A+J">Andrew J. Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Gawiser%2C+E">Eric Gawiser</a>, <a href="/search/astro-ph?searchtype=author&query=Gizis%2C+J">John Gizis</a>, <a href="/search/astro-ph?searchtype=author&query=Hlozek%2C+R">Renee Hlozek</a>, <a href="/search/astro-ph?searchtype=author&query=Kaviraj%2C+S">Sugata Kaviraj</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C+T">Charles T. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Lochner%2C+M">Michelle Lochner</a>, <a href="/search/astro-ph?searchtype=author&query=Mahabal%2C+A+A">Ashish A. Mahabal</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="2108.01683v2-abstract-short" style="display: inline;"> Vera C. Rubin Observatory is a ground-based astronomical facility under construction, a joint project of the National Science Foundation and the U.S. Department of Energy, designed to conduct a multi-purpose 10-year optical survey of the southern hemisphere sky: the Legacy Survey of Space and Time. Significant flexibility in survey strategy remains within the constraints imposed by the core scienc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.01683v2-abstract-full').style.display = 'inline'; document.getElementById('2108.01683v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.01683v2-abstract-full" style="display: none;"> Vera C. Rubin Observatory is a ground-based astronomical facility under construction, a joint project of the National Science Foundation and the U.S. Department of Energy, designed to conduct a multi-purpose 10-year optical survey of the southern hemisphere sky: the Legacy Survey of Space and Time. Significant flexibility in survey strategy remains within the constraints imposed by the core science goals of probing dark energy and dark matter, cataloging the Solar System, exploring the transient optical sky, and mapping the Milky Way. The survey's massive data throughput will be transformational for many other astrophysics domains and Rubin's data access policy sets the stage for a huge potential users' community. To ensure that the survey science potential is maximized while serving as broad a community as possible, Rubin Observatory has involved the scientific community at large in the process of setting and refining the details of the observing strategy. The motivation, history, and decision-making process of this strategy optimization are detailed in this paper, giving context to the science-driven proposals and recommendations for the survey strategy included in this Focus Issue. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.01683v2-abstract-full').style.display = 'none'; document.getElementById('2108.01683v2-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">Submitted as the opening paper of the Astrophysical Journal Focus Issue on Rubin LSST cadence and survey strategy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.02803">arXiv:2102.02803</a> <span> [<a href="https://arxiv.org/pdf/2102.02803">pdf</a>, <a href="https://arxiv.org/ps/2102.02803">ps</a>, <a href="https://arxiv.org/format/2102.02803">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/stab358">10.1093/mnras/stab358 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Principal component analysis tomography in near-infrared integral field spectroscopy of young stellar objects. I. Revisiting the high-mass protostar W33A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Navarete%2C+F">Felipe Navarete</a>, <a href="/search/astro-ph?searchtype=author&query=Damineli%2C+A">Augusto Damineli</a>, <a href="/search/astro-ph?searchtype=author&query=Steiner%2C+J+E">Jo茫o E. Steiner</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</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="2102.02803v1-abstract-short" style="display: inline;"> W33A is a well-known example of a high-mass young stellar object showing evidence of a circumstellar disc. We revisited the $K$-band NIFS/Gemini North observations of the W33A protostar using principal components analysis tomography and additional post-processing routines. Our results indicate the presence of a compact rotating disc based on the kinematics of the CO absorption features. The positi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.02803v1-abstract-full').style.display = 'inline'; document.getElementById('2102.02803v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.02803v1-abstract-full" style="display: none;"> W33A is a well-known example of a high-mass young stellar object showing evidence of a circumstellar disc. We revisited the $K$-band NIFS/Gemini North observations of the W33A protostar using principal components analysis tomography and additional post-processing routines. Our results indicate the presence of a compact rotating disc based on the kinematics of the CO absorption features. The position-velocity diagram shows that the disc exhibits a rotation curve with velocities that rapidly decrease for radii larger than 0\farcs1 ($\sim$250 AU) from the central source, suggesting a structure about four times more compact than previously reported. We derived a dynamical mass of 10.0$^{+4.1}_{-2.2}$ M$_\odot$ for the "disc+protostar" system, about $\sim$33% smaller than previously reported, but still compatible with high-mass protostar status. A relatively compact H$_2$ wind was identified at the base of the large-scale outflow of W33A, with a mean visual extinction of $\sim$63 mag. By taking advantage of supplementary near-infrared maps, we identified at least two other point-like objects driving extended structures in the vicinity of W33A, suggesting that multiple active protostars are located within the cloud. The closest object (Source B) was also identified in the NIFS field of view as a faint point-like object at a projected distance of $\sim$7,000 AU from W33A, powering extended $K$-band continuum emission detected in the same field. Another source (Source C) is driving a bipolar H$_2$ jet aligned perpendicular to the rotation axis of W33A. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.02803v1-abstract-full').style.display = 'none'; document.getElementById('2102.02803v1-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> 4 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">to appear on MNRAS. 24 pages, 24 figures and supplementary data available at CDS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.13943">arXiv:2011.13943</a> <span> [<a href="https://arxiv.org/pdf/2011.13943">pdf</a>, <a href="https://arxiv.org/format/2011.13943">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/abceb7">10.3847/1538-3881/abceb7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Second Data Release of the Survey of the MAgellanic Stellar History (SMASH) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D+L">David L. Nidever</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=Ruiz-Lara%2C+T">Tomas Ruiz-Lara</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+A+E">Amy E. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+L+C">L. Clifton Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+C+P+M">Cameron P. M. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</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=Gallart%2C+C">Carme Gallart</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=Martin%2C+N+F">Nicolas F. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Massana%2C+P">Pol Massana</a>, <a href="/search/astro-ph?searchtype=author&query=Monachesi%2C+A">Antonela Monachesi</a>, <a href="/search/astro-ph?searchtype=author&query=Noel%2C+N+E+D">Noelia E. D. Noel</a>, <a href="/search/astro-ph?searchtype=author&query=Sakowska%2C+J+D">Joanna D. Sakowska</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R+P">Roeland P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+A+R">Alistair R. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Zaritsky%2C+D">Dennis Zaritsky</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Conn%2C+B+C">Blair C. Conn</a>, <a href="/search/astro-ph?searchtype=author&query=de+Boer%2C+T+J+L">Thomas J. L. de Boer</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R+A">Robert A. Gruendl</a>, <a href="/search/astro-ph?searchtype=author&query=Monelli%2C+M">Matteo Monelli</a>, <a href="/search/astro-ph?searchtype=author&query=Munoz%2C+R+R">Ricardo R. Munoz</a> , et al. (10 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="2011.13943v1-abstract-short" style="display: inline;"> The Large and Small Magellanic Clouds (LMC and SMC) are the largest satellite galaxies of the Milky Way and close enough to allow for a detailed exploration of their structure and formation history. The Survey of the MAgellanic Stellar History (SMASH) is a community Dark Energy Camera (DECam) survey of the Magellanic Clouds using $\sim$50 nights to sample over $\sim$2400 deg$^2$ centered on the Cl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13943v1-abstract-full').style.display = 'inline'; document.getElementById('2011.13943v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.13943v1-abstract-full" style="display: none;"> The Large and Small Magellanic Clouds (LMC and SMC) are the largest satellite galaxies of the Milky Way and close enough to allow for a detailed exploration of their structure and formation history. The Survey of the MAgellanic Stellar History (SMASH) is a community Dark Energy Camera (DECam) survey of the Magellanic Clouds using $\sim$50 nights to sample over $\sim$2400 deg$^2$ centered on the Clouds at $\sim$20% filling factor (but with contiguous coverage in the central regions) and to depths of $\sim$24th mag in $ugriz$. The primary goals of SMASH are to map out the extended stellar peripheries of the Clouds and uncover their complicated interaction and accretion history as well as to derive spatially-resolved star formation histories of the central regions and create a "movie" of their past star formation. Here we announce the second SMASH public data release (DR2), which contains all 197 fully-calibrated DECam fields including the main body fields in the central regions. The DR2 data are available through the Astro Data Lab hosted by the NSF's National Optical-Infrared Astronomy Research Laboratory. We highlight three science cases that make use of the SMASH DR2 data and will be published in the future: (1) preliminary star formation histories of the LMC; (2) the search for Magellanic star clusters using citizen scientists; and, (3) photometric metallicities of Magellanic Cloud stars using the DECam $u$-band. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13943v1-abstract-full').style.display = 'none'; document.getElementById('2011.13943v1-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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, 9 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/2010.11284">arXiv:2010.11284</a> <span> [<a href="https://arxiv.org/pdf/2010.11284">pdf</a>, <a href="https://arxiv.org/format/2010.11284">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/10.3847/2515-5172/abc1dc">10.3847/2515-5172/abc1dc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Preliminary Target Selection for the DESI Milky Way Survey (MWS) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+A+P">Andrew P. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</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=Koposov%2C+S+E">Sergey E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+T">Ting Li</a>, <a href="/search/astro-ph?searchtype=author&query=Manser%2C+C">Christopher Manser</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=Rockosi%2C+C">Constance Rockosi</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+M">Mei-Yu Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Aguado%2C+D+S">David S. Aguado</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenstein%2C+D+J">Daniel J. Eisenstein</a>, <a href="/search/astro-ph?searchtype=author&query=Duan%2C+Y">Yutong Duan</a>, <a href="/search/astro-ph?searchtype=author&query=Eftekharzadeh%2C+S">Sarah Eftekharzadeh</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">Enrique Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">Robert Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Landriau%2C+M">Martin Landriau</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chien-Hsiu Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Levi%2C+M+E">Michael E. Levi</a>, <a href="/search/astro-ph?searchtype=author&query=Meisner%2C+A+M">Aaron M. Meisner</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=Najita%2C+J">Joan Najita</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">Knut Olsen</a> , et al. (9 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="2010.11284v1-abstract-short" style="display: inline;"> The DESI Milky Way Survey (MWS) will observe $\ge$8 million stars between $16 < r < 19$ mag, supplemented by observations of brighter targets under poor observing conditions. The survey will permit an accurate determination of stellar kinematics and population gradients; characterize diffuse substructure in the thick disk and stellar halo; enable the discovery of extremely metal-poor stars and oth… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.11284v1-abstract-full').style.display = 'inline'; document.getElementById('2010.11284v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.11284v1-abstract-full" style="display: none;"> The DESI Milky Way Survey (MWS) will observe $\ge$8 million stars between $16 < r < 19$ mag, supplemented by observations of brighter targets under poor observing conditions. The survey will permit an accurate determination of stellar kinematics and population gradients; characterize diffuse substructure in the thick disk and stellar halo; enable the discovery of extremely metal-poor stars and other rare stellar types; and improve constraints on the Galaxy's 3D dark matter distribution from halo star kinematics. MWS will also enable a detailed characterization of the stellar populations within 100 pc of the Sun, including a complete census of white dwarfs. The target catalog from the preliminary selection described here is public. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.11284v1-abstract-full').style.display = 'none'; document.getElementById('2010.11284v1-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 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">4 pages, 1 figure; published in Res. Notes AAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Res. Notes AAS, 4, 188 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.02308">arXiv:2009.02308</a> <span> [<a href="https://arxiv.org/pdf/2009.02308">pdf</a>, <a href="https://arxiv.org/format/2009.02308">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/stab298">10.1093/mnras/stab298 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Baryon Acoustic Oscillations in the projected cross-correlation function between the eBOSS DR16 quasars and photometric galaxies from the DESI Legacy Imaging Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zarrouk%2C+P">Pauline Zarrouk</a>, <a href="/search/astro-ph?searchtype=author&query=Rezaie%2C+M">Mehdi Rezaie</a>, <a href="/search/astro-ph?searchtype=author&query=Raichoor%2C+A">Anand Raichoor</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=Alam%2C+S">Shadab Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Brookes%2C+D">David Brookes</a>, <a href="/search/astro-ph?searchtype=author&query=Chuang%2C+C">Chia-Hsun Chuang</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K+S">Kyle S. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenstein%2C+D+J">Daniel J. Eisenstein</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">Robert Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Landriau%2C+M">Martin Landriau</a>, <a href="/search/astro-ph?searchtype=author&query=Moustakas%2C+J">John Moustakas</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=Norberg%2C+P">Peder Norberg</a>, <a href="/search/astro-ph?searchtype=author&query=Percival%2C+W+J">Will J. Percival</a>, <a href="/search/astro-ph?searchtype=author&query=Prada%2C+F">Francisco Prada</a>, <a href="/search/astro-ph?searchtype=author&query=Schubnell%2C+M">Michael Schubnell</a>, <a href="/search/astro-ph?searchtype=author&query=Seo%2C+H">Hee-Jong Seo</a>, <a href="/search/astro-ph?searchtype=author&query=Tarl%C3%A9%2C+G">Gregory Tarl茅</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+C">Cheng Zhao</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="2009.02308v1-abstract-short" style="display: inline;"> We search for the Baryon Acoustic Oscillations in the projected cross-correlation function binned into transverse comoving radius between the SDSS-IV DR16 eBOSS quasars and a dense photometric sample of galaxies selected from the DESI Legacy Imaging Surveys. We estimate the density of the photometric sample of galaxies in this redshift range to be about 2900 deg$^{-2}$, which is deeper than the of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.02308v1-abstract-full').style.display = 'inline'; document.getElementById('2009.02308v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.02308v1-abstract-full" style="display: none;"> We search for the Baryon Acoustic Oscillations in the projected cross-correlation function binned into transverse comoving radius between the SDSS-IV DR16 eBOSS quasars and a dense photometric sample of galaxies selected from the DESI Legacy Imaging Surveys. We estimate the density of the photometric sample of galaxies in this redshift range to be about 2900 deg$^{-2}$, which is deeper than the official DESI ELG selection, and the density of the spectroscopic sample is about 20 deg$^{-2}$. In order to mitigate the systematics related to the use of different imaging surveys close to the detection limit, we use a neural network approach that accounts for complex dependencies between the imaging attributes and the observed galaxy density. We find that we are limited by the depth of the imaging surveys which affects the density and purity of the photometric sample and its overlap in redshift with the quasar sample, which thus affects the performance of the method. When cross-correlating the photometric galaxies with quasars in $0.6 \leq z \leq 1.2$, the cross-correlation function can provide better constraints on the comoving angular distance, $D_{\rm M}$ (6\% precision) compared to the constraint on the spherically-averaged distance $D_{\rm V}$ (9\% precision) obtained from the auto-correlation. Although not yet competitive, this technique will benefit from the arrival of deeper photometric data from upcoming surveys which will enable it to go beyond the current limitations we have identified in this work. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.02308v1-abstract-full').style.display = 'none'; document.getElementById('2009.02308v1-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> 4 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">21 pages, 25 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/2005.13126">arXiv:2005.13126</a> <span> [<a href="https://arxiv.org/pdf/2005.13126">pdf</a>, <a href="https://arxiv.org/format/2005.13126">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/abc0f0">10.3847/1538-4357/abc0f0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The clustering of LRGs in the DECaLS DR8 footprint: distance constraints from baryon acoustic oscillations using photometric redshifts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sridhar%2C+S">Srivatsan Sridhar</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yong-Seon Song</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=Zhou%2C+R">Rongpu Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+J+A">Jeffrey A. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Chuang%2C+C">Chia-Hsun Chuang</a>, <a href="/search/astro-ph?searchtype=author&query=Prada%2C+F">Francisco Prada</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">Enrique Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Landriau%2C+M">Martin Landriau</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="2005.13126v1-abstract-short" style="display: inline;"> A photometric redshift sample of Luminous Red Galaxies (hereafter LRGs) obtained from The DECam Legacy Survey (DECaLS) is analysed to probe cosmic distances by exploiting the wedge approach of the two-point correlation function. Although the cosmological information is highly contaminated by the uncertainties existing in the photometric redshifts from the galaxy map, an angular diameter distance c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.13126v1-abstract-full').style.display = 'inline'; document.getElementById('2005.13126v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.13126v1-abstract-full" style="display: none;"> A photometric redshift sample of Luminous Red Galaxies (hereafter LRGs) obtained from The DECam Legacy Survey (DECaLS) is analysed to probe cosmic distances by exploiting the wedge approach of the two-point correlation function. Although the cosmological information is highly contaminated by the uncertainties existing in the photometric redshifts from the galaxy map, an angular diameter distance can be probed at the perpendicular configuration in which the measured correlation function is minimally contaminated. An ensemble of wedged correlation functions selected up to a given threshold based on having the least contamination was studied in the previous work (arXiv:1903.09651v2 [astro-ph.CO]) using simulations, and the extracted cosmological information was unbiased within this threshold. We apply the same methodology for analysing the LRG sample from DECaLS which will provide the optical imaging for targeting two-thirds of the DESI footprint and measure the angular diameter distances at $z=0.69$ and $z=0.87$ to be $D_{A}(0.697)=(1499 \pm 77\,\mathrm{Mpc})(r_{d}/r_{d,fid})$ and $D_{A}(0.874)=(1680 \pm 109\,\mathrm{Mpc})(r_{d}/r_{d,fid})$ with a fractional error of 5.14% and 6.48% respectively. We obtain a value of $H_{0}=67.59\pm5.52$ km/s/Mpc which supports the $H_0$ measured by all other BAO results and is consistent with $螞$CDM model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.13126v1-abstract-full').style.display = 'none'; document.getElementById('2005.13126v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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, 8 figures, DESI publication board APPROVED, submitted 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/2002.05828">arXiv:2002.05828</a> <span> [<a href="https://arxiv.org/pdf/2002.05828">pdf</a>, <a href="https://arxiv.org/format/2002.05828">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/ab93b9">10.3847/1538-3881/ab93b9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observing Strategy for the Legacy Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Burleigh%2C+K+J">Kaylan J. Burleigh</a>, <a href="/search/astro-ph?searchtype=author&query=Landriau%2C+M">Martin Landriau</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Lang%2C+D">Dustin Lang</a>, <a href="/search/astro-ph?searchtype=author&query=Schlegel%2C+D+J">David J. Schlegel</a>, <a href="/search/astro-ph?searchtype=author&query=Nugent%2C+P+E">Peter E. Nugent</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Findlay%2C+J+R">Joseph R. Findlay</a>, <a href="/search/astro-ph?searchtype=author&query=Finkbeiner%2C+D+P">Douglas P. Finkbeiner</a>, <a href="/search/astro-ph?searchtype=author&query=Herrera%2C+D">David Herrera</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">Klaus Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">St茅phanie Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=McGreer%2C+I">Ian McGreer</a>, <a href="/search/astro-ph?searchtype=author&query=Meisner%2C+A+M">Aaron M. Meisner</a>, <a href="/search/astro-ph?searchtype=author&query=Moustakas%2C+J">John Moustakas</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=Patej%2C+A">Anna Patej</a>, <a href="/search/astro-ph?searchtype=author&query=Schlafly%2C+E+F">Edward F. Schlafly</a>, <a href="/search/astro-ph?searchtype=author&query=Valdes%2C+F">Francisco Valdes</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+A+R">Alistair R. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Weaver%2C+B+A">Benjamin A. Weaver</a>, <a href="/search/astro-ph?searchtype=author&query=Y%C3%A8che%2C+C">Christophe Y猫che</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="2002.05828v2-abstract-short" style="display: inline;"> The Legacy Surveys, a combination of three ground-based imaging surveys, have mapped 16,000 deg$^2$ in three optical bands ($g$, $r$, and $z$) to a depth 1--$2$~mag deeper than the Sloan Digital Sky Survey (SDSS). Our work addresses one of the major challenges of wide-field imaging surveys conducted at ground-based observatories: the varying depth that results from varying observing conditions at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.05828v2-abstract-full').style.display = 'inline'; document.getElementById('2002.05828v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.05828v2-abstract-full" style="display: none;"> The Legacy Surveys, a combination of three ground-based imaging surveys, have mapped 16,000 deg$^2$ in three optical bands ($g$, $r$, and $z$) to a depth 1--$2$~mag deeper than the Sloan Digital Sky Survey (SDSS). Our work addresses one of the major challenges of wide-field imaging surveys conducted at ground-based observatories: the varying depth that results from varying observing conditions at Earth-bound sites. To mitigate these effects, two of the Legacy Surveys (the Dark Energy Camera Legacy Survey, or DECaLS; and the Mayall $z$-band Legacy Survey, or MzLS) employed a unique strategy to dynamically adjust the exposure times as rapidly as possible in response to the changing observing conditions. We present the tiling and observing strategies used by these surveys. We demonstrate that the tiling and dynamic observing strategies jointly result in a more uniform-depth survey that has higher efficiency for a given total observing time compared with the traditional approach of using fixed exposure times. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.05828v2-abstract-full').style.display = 'none'; document.getElementById('2002.05828v2-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> 9 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">v1: 14 pages, 3 tables and 5 figures; v2: 15 pages, 3 tables and 6 figures. Changes in response to referee comments; matches published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> AJ, 160:61 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.11417">arXiv:1908.11417</a> <span> [<a href="https://arxiv.org/pdf/1908.11417">pdf</a>, <a href="https://arxiv.org/format/1908.11417">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> <p class="title is-5 mathjax"> Infrastructure and Strategies for Time Domain and MMA and Follow-Up </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Miller%2C+B+W">B. W. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+L">L. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Bellm%2C+E">E. Bellm</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F">F. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J">J. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">R. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Bolton%2C+A">A. Bolton</a>, <a href="/search/astro-ph?searchtype=author&query=Briceno%2C+C">C. Briceno</a>, <a href="/search/astro-ph?searchtype=author&query=Clarkson%2C+W">W. Clarkson</a>, <a href="/search/astro-ph?searchtype=author&query=Elias%2C+J">J. Elias</a>, <a href="/search/astro-ph?searchtype=author&query=Gezari%2C+S">S. Gezari</a>, <a href="/search/astro-ph?searchtype=author&query=Goodrich%2C+B">B. Goodrich</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+M+J">M. J. Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+M+L">M. L. Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Heathcote%2C+S">S. Heathcote</a>, <a href="/search/astro-ph?searchtype=author&query=Hsieh%2C+H">H. Hsieh</a>, <a href="/search/astro-ph?searchtype=author&query=Lotz%2C+J">J. Lotz</a>, <a href="/search/astro-ph?searchtype=author&query=Matheson%2C+T">Tom Matheson</a>, <a href="/search/astro-ph?searchtype=author&query=McSwain%2C+M+V">M. V. McSwain</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+D">D. Norman</a>, <a href="/search/astro-ph?searchtype=author&query=Rector%2C+T">T. Rector</a>, <a href="/search/astro-ph?searchtype=author&query=Riddle%2C+R">R. Riddle</a>, <a href="/search/astro-ph?searchtype=author&query=Ridgway%2C+S">S. Ridgway</a>, <a href="/search/astro-ph?searchtype=author&query=Saha%2C+A">A. Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Street%2C+R">R. Street</a> , et al. (6 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="1908.11417v1-abstract-short" style="display: inline;"> Time domain and multi-messenger astrophysics are growing and important modes of observational astronomy that will help define astrophysics in the 2020s. Significant effort is being put into developing the components of a follow-up system for dynamically turning survey alerts into data. This system consists of: 1) brokers that will aggregate, classify, and filter alerts; 2) Target Observation Manag… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.11417v1-abstract-full').style.display = 'inline'; document.getElementById('1908.11417v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.11417v1-abstract-full" style="display: none;"> Time domain and multi-messenger astrophysics are growing and important modes of observational astronomy that will help define astrophysics in the 2020s. Significant effort is being put into developing the components of a follow-up system for dynamically turning survey alerts into data. This system consists of: 1) brokers that will aggregate, classify, and filter alerts; 2) Target Observation Managers (TOMs) for prioritizing targets and managing observations and data; and 3) observatory interfaces, schedulers, and facilities along with data reduction software and science archives. These efforts need continued community support and funding in order to complete and maintain them. Many of the efforts can be community open-source software projects but they will benefit from the leadership of professional software developers. The coordination should be done by institutions that are involved in the follow-up system such as the national observatories (e.g. LSST/Gemini/NOAO Mid-scale/Community Science and Data Center) or a new MMA institute. These tools will help the community to produce the most science from new facilities and will provide new capabilities for all users of the facilities that adopt them. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.11417v1-abstract-full').style.display = 'none'; document.getElementById('1908.11417v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Astro2020 Decadal Survey Activities, Projects, or State of the Profession Consideration (APC) white paper</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.10487">arXiv:1907.10487</a> <span> [<a href="https://arxiv.org/pdf/1907.10487">pdf</a>, <a href="https://arxiv.org/ps/1907.10487">ps</a>, <a href="https://arxiv.org/format/1907.10487">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> <p class="title is-5 mathjax"> Future Uses of the LSST Facility: Input from the LSST Project Science Team </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kahn%2C+S">S. Kahn</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Claver%2C+C">Chuck Claver</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+A">Andrew Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+L">Leanne Guy</a>, <a href="/search/astro-ph?searchtype=author&query=Ivezi%C4%87%2C+%C5%BD">沤eljko Ivezi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Lupton%2C+R+H">Robert H. Lupton</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Mullane%2C+W">William O'Mullane</a>, <a href="/search/astro-ph?searchtype=author&query=Ritz%2C+S">Steven Ritz</a>, <a href="/search/astro-ph?searchtype=author&query=Strauss%2C+M">Michael Strauss</a>, <a href="/search/astro-ph?searchtype=author&query=Stubbs%2C+C">Christopher Stubbs</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+S+J">Sandrine J. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Tyson%2C+J+A">J. Anthony Tyson</a>, <a href="/search/astro-ph?searchtype=author&query=Xin%2C+B">Bo Xin</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="1907.10487v1-abstract-short" style="display: inline;"> In this white paper, we discuss future uses of the LSST facility after the planned 10-year survey is complete. We expect the LSST survey to profoundly affect the scientific landscape over the next ten years, and it is likely that unexpected discoveries may drive its future scientific program. We discuss various operations and instrument options that could be considered for an extended LSST mission… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.10487v1-abstract-full').style.display = 'inline'; document.getElementById('1907.10487v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.10487v1-abstract-full" style="display: none;"> In this white paper, we discuss future uses of the LSST facility after the planned 10-year survey is complete. We expect the LSST survey to profoundly affect the scientific landscape over the next ten years, and it is likely that unexpected discoveries may drive its future scientific program. We discuss various operations and instrument options that could be considered for an extended LSST mission beyond ten years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.10487v1-abstract-full').style.display = 'none'; document.getElementById('1907.10487v1-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 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">10 pages, no figures. arXiv admin note: text overlap with arXiv:1905.04669</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.02264">arXiv:1907.02264</a> <span> [<a href="https://arxiv.org/pdf/1907.02264">pdf</a>, <a href="https://arxiv.org/format/1907.02264">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/10.1051/0004-6361/201936021">10.1051/0004-6361/201936021 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the nature of a shell of young stars in the outskirts of the Small Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martinez-Delgado%2C+D">David Martinez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Vivas%2C+A+K">A. Katherina Vivas</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E+K">Eva K. Grebel</a>, <a href="/search/astro-ph?searchtype=author&query=Gallart%2C+C">Carme Gallart</a>, <a href="/search/astro-ph?searchtype=author&query=Pieres%2C+A">Adriano Pieres</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+C+P+M">Cameron P. M. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Zivick%2C+P">Paul Zivick</a>, <a href="/search/astro-ph?searchtype=author&query=Lemasle%2C+B">Bertrand Lemasle</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+L+C">L. Clifton Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Carballo-Bello%2C+J+A">Julio A. Carballo-Bello</a>, <a href="/search/astro-ph?searchtype=author&query=Noel%2C+N+E+D">Noelia E. D. Noel</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=Choi%2C+Y">Yumi Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">Gurtina Besla</a>, <a href="/search/astro-ph?searchtype=author&query=Schmidt%2C+J">Judy Schmidt</a>, <a href="/search/astro-ph?searchtype=author&query=Zaritsky%2C+D">Dennis Zaritsky</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R+A">Robert A. Gruendl</a>, <a href="/search/astro-ph?searchtype=author&query=Seibert%2C+M">Mark Seibert</a>, <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D">David Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Monteagudo%2C+L">Laura Monteagudo</a>, <a href="/search/astro-ph?searchtype=author&query=Monelli%2C+M">Mateo Monelli</a>, <a href="/search/astro-ph?searchtype=author&query=Hubl%2C+B">Bernhard Hubl</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R">Roeland van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Ballesteros%2C+F+J">Fernando J. Ballesteros</a>, <a href="/search/astro-ph?searchtype=author&query=Stringfellow%2C+G">Guy Stringfellow</a> , et al. (13 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="1907.02264v2-abstract-short" style="display: inline;"> Understanding the evolutionary history of the Magellanic Clouds requires an in-depth exploration and characterization of the stellar content in their outer regions, which ultimately are key to tracing the epochs and nature of past interactions. We present new deep images of a shell-like over-density of stars in the outskirts of the Small Magellanic Cloud (SMC). The shell, also detected in photogra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.02264v2-abstract-full').style.display = 'inline'; document.getElementById('1907.02264v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.02264v2-abstract-full" style="display: none;"> Understanding the evolutionary history of the Magellanic Clouds requires an in-depth exploration and characterization of the stellar content in their outer regions, which ultimately are key to tracing the epochs and nature of past interactions. We present new deep images of a shell-like over-density of stars in the outskirts of the Small Magellanic Cloud (SMC). The shell, also detected in photographic plates dating back to the fifties, is located at ~1.9 degr from the center of the SMC in the north-east direction.The structure and stellar content of this feature were studied with multi-band, optical data from the Survey of the MAgellanic Stellar History (SMASH) carried out with the Dark Energy Camera on the Blanco Telescope at Cerro Tololo Inter-American Observatory. We also investigate the kinematic of the stars in the shell using the Gaia Data Release 2. The shell is composed of a young population with an age ~ 150 Myr, with no contribution from an old population. Thus, it is hard to explain its origin as the remnant of a tidally disrupted stellar system. The spatial distribution of the young main-sequence stars shows a rich sub-structure, with a spiral arm-like feature emanating from the main shell and a separated small arc of young stars close to the globular cluster NGC 362. We find that the absolute g-band magnitude of the shell is M_{g,shell} = -10.78+/- 0.02, with a surface brightness of mu_{g,shell} = 25.81+/- 0.01 mag/arcsec^{2}. We have not found any evidence that this feature is of tidal origin or a bright part of a spiral arm-like structure. Instead, we suggest that the shell formed in a recent star formation event, likely triggered by an interaction with the Large Magellanic Cloud and/or the Milky Way, ~150 Myr ago. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.02264v2-abstract-full').style.display = 'none'; document.getElementById('1907.02264v2-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">16 pages, 14 figures, submitted to Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 631, A98 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.05637">arXiv:1902.05637</a> <span> [<a href="https://arxiv.org/pdf/1902.05637">pdf</a>, <a href="https://arxiv.org/format/1902.05637">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/ab07ba">10.3847/1538-4357/ab07ba <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mapping the Interstellar Reddening and Extinction towards Baade's Window Using Minimum Light Colors of ab-type RR Lyrae Stars. Revelations from the De-reddened Color-Magnitude Diagrams </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saha%2C+A">Abhijit Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Vivas%2C+A+K">A. Katherina Vivas</a>, <a href="/search/astro-ph?searchtype=author&query=Olszewski%2C+E+W">Edward W. Olszewski</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+V">Verne Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">Knut Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Valdes%2C+F">Francisco Valdes</a>, <a href="/search/astro-ph?searchtype=author&query=Claver%2C+J">Jenna Claver</a>, <a href="/search/astro-ph?searchtype=author&query=Calamida%2C+A">Annalisa Calamida</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+A+R">Alistair R. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Matheson%2C+T">Thomas Matheson</a>, <a href="/search/astro-ph?searchtype=author&query=Narayan%2C+G">Gautham Narayan</a>, <a href="/search/astro-ph?searchtype=author&query=Soraisam%2C+M">Monika Soraisam</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">T. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Bloom%2C+J+S">Joshua S. Bloom</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. Bradley Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">Brenda Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Juric%2C+M">Mario Juric</a>, <a href="/search/astro-ph?searchtype=author&query=Kaleida%2C+C">Catherine Kaleida</a>, <a href="/search/astro-ph?searchtype=author&query=Kunder%2C+A">Andrea Kunder</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+A">Adam Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D">David Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Ridgway%2C+S">Stephen Ridgway</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="1902.05637v1-abstract-short" style="display: inline;"> We have obtained repeated images of 6 fields towards the Galactic bulge in 5 passbands (u, g, r, i, z) with the DECam imager on the Blanco 4m telescope at CTIO. From over 1.6 billion individual photometric measurements in the field centered on Baade's window, we have detected 4877 putative variable stars. 474 of these have been confirmed as fundamental mode RR Lyrae stars, whose colors at minimum… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.05637v1-abstract-full').style.display = 'inline'; document.getElementById('1902.05637v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.05637v1-abstract-full" style="display: none;"> We have obtained repeated images of 6 fields towards the Galactic bulge in 5 passbands (u, g, r, i, z) with the DECam imager on the Blanco 4m telescope at CTIO. From over 1.6 billion individual photometric measurements in the field centered on Baade's window, we have detected 4877 putative variable stars. 474 of these have been confirmed as fundamental mode RR Lyrae stars, whose colors at minimum light yield line-of-sight reddening determinations as well as a reddening law towards the Galactic Bulge which differs significantly from the standard R_V = 3.1 formulation. Assuming that the stellar mix is invariant over the 3 square-degree field, we are able to derive a line-of-sight reddening map with sub-arcminute resolution, enabling us to obtain de-reddened and extinction corrected color-magnitude diagrams (CMD's) of this bulge field using up to 2.5 million well-measured stars. The corrected CMD's show unprecedented detail and expose sparsely populated sequences: e.g., delineation of the very wide red giant branch, structure within the red giant clump, the full extent of the horizontal branch, and a surprising bright feature which is likely due to stars with ages younger than 1 Gyr. We use the RR Lyrae stars to trace the spatial structure of the ancient stars, and find an exponential decline in density with Galactocentric distance. We discuss ways in which our data products can be used to explore the age and metallicity properties of the bulge, and how our larger list of all variables is useful for learning to interpret future LSST alerts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.05637v1-abstract-full').style.display = 'none'; document.getElementById('1902.05637v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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 for publication in AAS journals; most likely The Astrophysical 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/1812.02932">arXiv:1812.02932</a> <span> [<a href="https://arxiv.org/pdf/1812.02932">pdf</a>, <a href="https://arxiv.org/format/1812.02932">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> <p class="title is-5 mathjax"> Unveiling the Rich and Diverse Universe of Subsecond Astrophysics through LSST Star Trails </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+D">David Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Kahn%2C+S+M">Steven M. Kahn</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">Federica B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Ivezi%C4%87%2C+%C5%BD">沤eljko Ivezi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">Claudia M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">Andrea Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+J+R">John R. Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+C+J">Colin J. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Jacoby%2C+G+H">George H. Jacoby</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+S+B">Steve B. Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Madejski%2C+G">Grzegorz Madejski</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="1812.02932v1-abstract-short" style="display: inline;"> We present a unique method that allows the LSST to scan the sky for stellar variability on short timescales. The operational component of the strategy requires LSST to take star trail images. The image processing component uses deep learning to sift for transient events on timescales down to 10 ms. We advocate for enabling this observing mode with LSST, as coupling this capability with the LSST's… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.02932v1-abstract-full').style.display = 'inline'; document.getElementById('1812.02932v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.02932v1-abstract-full" style="display: none;"> We present a unique method that allows the LSST to scan the sky for stellar variability on short timescales. The operational component of the strategy requires LSST to take star trail images. The image processing component uses deep learning to sift for transient events on timescales down to 10 ms. We advocate for enabling this observing mode with LSST, as coupling this capability with the LSST's tremendous 319.5 m$^2$deg$^2$ etendue will produce the first wide area optical survey of the universe on these timescales. We explain how these data will advance both planned lines of investigation and enable new research in the areas of stellar flares, cataclysmic variables, active galactic nuclei, Kuiper Belt objects, gamma-ray bursts, and fast radio bursts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.02932v1-abstract-full').style.display = 'none'; document.getElementById('1812.02932v1-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> 7 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.02671">arXiv:1805.02671</a> <span> [<a href="https://arxiv.org/pdf/1805.02671">pdf</a>, <a href="https://arxiv.org/format/1805.02671">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/aafaf7">10.3847/1538-4357/aafaf7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the Very Extended Low Surface Brightness Stellar Populations of the Large Magellanic Cloud with SMASH </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D+L">David L. Nidever</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=de+Boer%2C+T+J+L">Thomas J. L. de Boer</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Zaritsky%2C+D">Dennis Zaritsky</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Saha%2C+A">Abhijit Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Conn%2C+B+C">Blair C. Conn</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">Gurtina Besla</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R+P">Roeland P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Noel%2C+N+E+D">Noelia E. D. Noel</a>, <a href="/search/astro-ph?searchtype=author&query=Monachesi%2C+A">Antonela Monachesi</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=Massana%2C+P">Pol Massana</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=Gallart%2C+C">Carme Gallart</a>, <a href="/search/astro-ph?searchtype=author&query=Monelli%2C+M">Matteo Monelli</a>, <a href="/search/astro-ph?searchtype=author&query=Martinez-Delgado%2C+D">David Martinez-Delgado</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=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Vivas%2C+A+K">A. Katherina Vivas</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+A+R">Alistair R. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Kaleida%2C+C">Catherine Kaleida</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="1805.02671v1-abstract-short" style="display: inline;"> We present the detection of very extended stellar populations around the Large Magellanic Cloud (LMC) out to R~21 degrees, or ~18.5 kpc at the LMC distance of 50 kpc, as detected in the Survey of the MAgellanic Stellar History (SMASH) performed with the Dark Energy Camera on the NOAO Blanco 4m Telescope. The deep (g~24) SMASH color magnitude diagrams (CMDs) clearly reveal old (~9 Gyr), metal-poor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.02671v1-abstract-full').style.display = 'inline'; document.getElementById('1805.02671v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.02671v1-abstract-full" style="display: none;"> We present the detection of very extended stellar populations around the Large Magellanic Cloud (LMC) out to R~21 degrees, or ~18.5 kpc at the LMC distance of 50 kpc, as detected in the Survey of the MAgellanic Stellar History (SMASH) performed with the Dark Energy Camera on the NOAO Blanco 4m Telescope. The deep (g~24) SMASH color magnitude diagrams (CMDs) clearly reveal old (~9 Gyr), metal-poor ([Fe/H]=-0.8 dex) main-sequence stars at a distance of 50 kpc. The surface brightness of these detections is extremely low with our most distant detection having 34 mag per arcsec squared in g-band. The SMASH radial density profile breaks from the inner LMC exponential decline at ~13-15 degrees and a second component at larger radii has a shallower slope with power-law index of -2.2 that contributes ~0.4% of the LMC's total stellar mass. In addition, the SMASH densities exhibit large scatter around our best-fit model of ~70% indicating that the envelope of stellar material in the LMC periphery is highly disturbed. We also use data from the NOAO Source catalog to map the LMC main-sequence populations at intermediate radii and detect a steep dropoff in density on the eastern side of the LMC (at R~8 deg) as well as an extended structure to the far northeast. These combined results confirm the existence of a very extended, low-density envelope of stellar material with disturbed shape around the LMC. The exact origin of this structure remains unclear but the leading options include a classical accreted halo or tidally stripped outer disk material. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.02671v1-abstract-full').style.display = 'none'; document.getElementById('1805.02671v1-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> 7 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2018. </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">9 pages, 5 figues, 1 table, submitted 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/1805.00481">arXiv:1805.00481</a> <span> [<a href="https://arxiv.org/pdf/1805.00481">pdf</a>, <a href="https://arxiv.org/format/1805.00481">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/aaed1f">10.3847/1538-4357/aaed1f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SMASHing THE LMC: Mapping a Ring-like Stellar Overdensity in the LMC Disk </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Choi%2C+Y">Yumi Choi</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=Olsen%2C+K">Knut Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">Gurtina Besla</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Zaritsky%2C+D">Dennis Zaritsky</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=van+der+Marel%2C+R+P">Roeland P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+L+C">L. Clifton Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Vivas%2C+A+K">A. Katherina Vivas</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+A+R">Alistair R. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=de+Boer%2C+T+J+L">Thomas J. L. de Boer</a>, <a href="/search/astro-ph?searchtype=author&query=Noel%2C+N+E+D">Noelia E. D. Noel</a>, <a href="/search/astro-ph?searchtype=author&query=Monachesi%2C+A">Antonela Monachesi</a>, <a href="/search/astro-ph?searchtype=author&query=Gallart%2C+C">Carme Gallart</a>, <a href="/search/astro-ph?searchtype=author&query=Monelli%2C+M">Matteo Monelli</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=Massana%2C+P">Pol Massana</a>, <a href="/search/astro-ph?searchtype=author&query=Martinez-Delgado%2C+D">David Martinez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Munoz%2C+R">Ricardo Munoz</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="1805.00481v2-abstract-short" style="display: inline;"> We explore the stellar structure of the Large Magellanic Cloud (LMC) disk using data from the Survey of the MAgellanic Stellar History (SMASH) and the Dark Energy Survey. We detect a ring-like stellar overdensity in the red clump star count map at a radius of ~6 degrees (~5.2 kpc at the LMC distance) that is continuous over ~270 degrees in position angle and is only limited by the current data cov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.00481v2-abstract-full').style.display = 'inline'; document.getElementById('1805.00481v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.00481v2-abstract-full" style="display: none;"> We explore the stellar structure of the Large Magellanic Cloud (LMC) disk using data from the Survey of the MAgellanic Stellar History (SMASH) and the Dark Energy Survey. We detect a ring-like stellar overdensity in the red clump star count map at a radius of ~6 degrees (~5.2 kpc at the LMC distance) that is continuous over ~270 degrees in position angle and is only limited by the current data coverage. The overdensity shows an amplitude up to 2.5 times higher than that of the underlying smooth disk. This structure might be related to the multiple arms found by de Vaucouleurs. We find that the overdensity shows spatial correlation with intermediate-age star clusters, but not with young (< 1 Gyr) main-sequence stars, indicating the stellar populations associated with the overdensity are intermediate in age or older. Our findings on the LMC overdensity can be explained by either of two distinct formation mechanisms of a ring-like overdensity: (1) the overdensity formed out of an asymmetric one-armed spiral wrapping around the LMC main body, which is induced by repeated encounters with the Small Magellanic Cloud (SMC) over the last Gyr, or (2) the overdensity formed very recently as a tidal response to a direct collision with the SMC. Although the measured properties of the overdensity alone cannot distinguish between the two candidate scenarios, the consistency with both scenarios suggests that the ring-like overdensity is likely a product of tidal interaction with the SMC, but not with the Milky Way halo. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.00481v2-abstract-full').style.display = 'none'; document.getElementById('1805.00481v2-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 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2018. </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, 4 figures, 1 table, Published in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2018 ApJ, 869, 125 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.08657">arXiv:1804.08657</a> <span> [<a href="https://arxiv.org/pdf/1804.08657">pdf</a>, <a href="https://arxiv.org/format/1804.08657">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/ab089d">10.3847/1538-3881/ab089d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Overview of the DESI Legacy Imaging Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Schlegel%2C+D+J">David J. Schlegel</a>, <a href="/search/astro-ph?searchtype=author&query=Lang%2C+D">Dustin Lang</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Burleigh%2C+K">Kaylan Burleigh</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">Xiaohui Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Findlay%2C+J+R">Joseph R. Findlay</a>, <a href="/search/astro-ph?searchtype=author&query=Finkbeiner%2C+D">Doug Finkbeiner</a>, <a href="/search/astro-ph?searchtype=author&query=Herrera%2C+D">David Herrera</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">Stephanie Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Landriau%2C+M">Martin Landriau</a>, <a href="/search/astro-ph?searchtype=author&query=Levi%2C+M">Michael Levi</a>, <a href="/search/astro-ph?searchtype=author&query=McGreer%2C+I">Ian McGreer</a>, <a href="/search/astro-ph?searchtype=author&query=Meisner%2C+A">Aaron Meisner</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=Moustakas%2C+J">John Moustakas</a>, <a href="/search/astro-ph?searchtype=author&query=Nugent%2C+P">Peter Nugent</a>, <a href="/search/astro-ph?searchtype=author&query=Patej%2C+A">Anna Patej</a>, <a href="/search/astro-ph?searchtype=author&query=Schlafly%2C+E+F">Edward F. Schlafly</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+A+R">Alistair R. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Valdes%2C+F">Francisco Valdes</a>, <a href="/search/astro-ph?searchtype=author&query=Weaver%2C+B+A">Benjamin A. Weaver</a>, <a href="/search/astro-ph?searchtype=author&query=Zou%2C+C+Y+H">Christophe Yeche Hu Zou</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+X">Xu Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Abareshi%2C+B">Behzad Abareshi</a> , et al. (135 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="1804.08657v2-abstract-short" style="display: inline;"> The DESI Legacy Imaging Surveys are a combination of three public projects (the Dark Energy Camera Legacy Survey, the Beijing-Arizona Sky Survey, and the Mayall z-band Legacy Survey) that will jointly image approximately 14,000 deg^2 of the extragalactic sky visible from the northern hemisphere in three optical bands (g, r, and z) using telescopes at the Kitt Peak National Observatory and the Cerr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.08657v2-abstract-full').style.display = 'inline'; document.getElementById('1804.08657v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.08657v2-abstract-full" style="display: none;"> The DESI Legacy Imaging Surveys are a combination of three public projects (the Dark Energy Camera Legacy Survey, the Beijing-Arizona Sky Survey, and the Mayall z-band Legacy Survey) that will jointly image approximately 14,000 deg^2 of the extragalactic sky visible from the northern hemisphere in three optical bands (g, r, and z) using telescopes at the Kitt Peak National Observatory and the Cerro Tololo Inter-American Observatory. The combined survey footprint is split into two contiguous areas by the Galactic plane. The optical imaging is conducted using a unique strategy of dynamically adjusting the exposure times and pointing selection during observing that results in a survey of nearly uniform depth. In addition to calibrated images, the project is delivering a catalog, constructed by using a probabilistic inference-based approach to estimate source shapes and brightnesses. The catalog includes photometry from the grz optical bands and from four mid-infrared bands (at 3.4, 4.6, 12 and 22 micorons) observed by the Wide-field Infrared Survey Explorer (WISE) satellite during its full operational lifetime. The project plans two public data releases each year. All the software used to generate the catalogs is also released with the data. This paper provides an overview of the Legacy Surveys project. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.08657v2-abstract-full').style.display = 'none'; document.getElementById('1804.08657v2-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 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </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">47 pages, 18 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/1804.07765">arXiv:1804.07765</a> <span> [<a href="https://arxiv.org/pdf/1804.07765">pdf</a>, <a href="https://arxiv.org/format/1804.07765">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/aae083">10.3847/1538-4357/aae083 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SMASHing the LMC: A Tidally-induced Warp in the Outer LMC and a Large-scale Reddening Map </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Choi%2C+Y">Yumi Choi</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=Olsen%2C+K">Knut Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">Gurtina Besla</a>, <a href="/search/astro-ph?searchtype=author&query=Zaritsky%2C+D">Dennis Zaritsky</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R+P">Roeland P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Gallart%2C+C">Carme Gallart</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=Johnson%2C+L+C">L. Clifton Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Vivas%2C+A+K">A. Katherina Vivas</a>, <a href="/search/astro-ph?searchtype=author&query=Saha%2C+A">Abhijit Saha</a>, <a href="/search/astro-ph?searchtype=author&query=de+Boer%2C+T+J+L">Thomas J. L. de Boer</a>, <a href="/search/astro-ph?searchtype=author&query=Noel%2C+N+E+D">Noelia E. D. Noel</a>, <a href="/search/astro-ph?searchtype=author&query=Monachesi%2C+A">Antonela Monachesi</a>, <a href="/search/astro-ph?searchtype=author&query=Massana%2C+P">Pol Massana</a>, <a href="/search/astro-ph?searchtype=author&query=Conn%2C+B+C">Blair C. Conn</a>, <a href="/search/astro-ph?searchtype=author&query=Martinez-Delgado%2C+D">David Martinez-Delgado</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=Stringfellow%2C+G">Guy Stringfellow</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="1804.07765v2-abstract-short" style="display: inline;"> We present a study of the three-dimensional (3D) structure of the Large Magellanic Cloud (LMC) using ~2.2 million red clump (RC) stars selected from the Survey of the MAgellanic Stellar History. To correct for line-of-sight dust extinction, the intrinsic RC color and magnitude and their radial dependence are carefully measured by using internal nearly dust-free regions. These are then used to cons… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.07765v2-abstract-full').style.display = 'inline'; document.getElementById('1804.07765v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.07765v2-abstract-full" style="display: none;"> We present a study of the three-dimensional (3D) structure of the Large Magellanic Cloud (LMC) using ~2.2 million red clump (RC) stars selected from the Survey of the MAgellanic Stellar History. To correct for line-of-sight dust extinction, the intrinsic RC color and magnitude and their radial dependence are carefully measured by using internal nearly dust-free regions. These are then used to construct an accurate 2D reddening map (165 square degrees with ~10 arcmin resolution) of the LMC disk and the 3D spatial distribution of RC stars. An inclined disk model is fit to the 2D distance map yielding a best-fit inclination angle i = 25.86(+0.73,-1.39) degrees with random errors of +\-0.19 degrees and line-of-nodes position angle theta = 149.23(+6.43,-8.35) degrees with random errors of +/-0.49 degrees. These angles vary with galactic radius, indicating that the LMC disk is warped and twisted likely due to the repeated tidal interactions with the Small Magellanic Cloud (SMC). For the first time, our data reveal a significant warp in the southwestern part of the outer disk starting at rho ~ 7 degrees that departs from the defined LMC plane up to ~4 kpc toward the SMC, suggesting that it originated from a strong interaction with the SMC. In addition, the inner disk encompassing the off-centered bar appears to be tilted up to 5-15 degrees relative to the rest of the LMC disk. These findings on the outer warp and the tilted bar are consistent with the predictions from the Besla et al. simulation of a recent direct collision with the SMC. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.07765v2-abstract-full').style.display = 'none'; document.getElementById('1804.07765v2-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 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </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, 15 figures, published in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2018 ApJ, 866, 90 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.03954">arXiv:1707.03954</a> <span> [<a href="https://arxiv.org/pdf/1707.03954">pdf</a>, <a href="https://arxiv.org/ps/1707.03954">ps</a>, <a href="https://arxiv.org/format/1707.03954">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/10.3847/1538-3881/aa7fed">10.3847/1538-3881/aa7fed <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Absolute Magnitudes and Colors of RR Lyrae stars in DECam Passbands from Photometry of the Globular Cluster M5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vivas%2C+A+K">A. Katherina Vivas</a>, <a href="/search/astro-ph?searchtype=author&query=Saha%2C+A">Abhijit Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">Knut Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Olszewski%2C+E+W">Edward W. Olszewski</a>, <a href="/search/astro-ph?searchtype=author&query=Claver%2C+J">Jennifer Claver</a>, <a href="/search/astro-ph?searchtype=author&query=Valdes%2C+F">Francisco Valdes</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">Tim Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Kaleida%2C+C">Catherine Kaleida</a>, <a href="/search/astro-ph?searchtype=author&query=Kunder%2C+A">Andrea Kunder</a>, <a href="/search/astro-ph?searchtype=author&query=Narayan%2C+G">Gautham Narayan</a>, <a href="/search/astro-ph?searchtype=author&query=Matheson%2C+T">Thomas Matheson</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+A">Alistair Walker</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="1707.03954v1-abstract-short" style="display: inline;"> We characterize the absolute magnitudes and colors of RR Lyrae stars in the globular cluster M5 in the ugriz filter system of the Dark Energy Camera (DECam). We provide empirical Period-Luminosity (P-L) relationships in all 5 bands based on 47 RR Lyrae stars of the type ab and 14 stars of the type c. The P-L relationships were found to be better constrained for the fundamental mode RR Lyrae stars… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.03954v1-abstract-full').style.display = 'inline'; document.getElementById('1707.03954v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.03954v1-abstract-full" style="display: none;"> We characterize the absolute magnitudes and colors of RR Lyrae stars in the globular cluster M5 in the ugriz filter system of the Dark Energy Camera (DECam). We provide empirical Period-Luminosity (P-L) relationships in all 5 bands based on 47 RR Lyrae stars of the type ab and 14 stars of the type c. The P-L relationships were found to be better constrained for the fundamental mode RR Lyrae stars in the riz passbands, with dispersion of 0.03, 0.02 and 0.02 magnitudes, respectively. The dispersion of the color at minimum light was found to be small, supporting the use of this parameter as a means to obtain accurate interstellar extinctions along the line of sight up to the distance of the RR Lyrae star. We found a trend of color at minimum light with pulsational period that, if taken into account, brings the dispersion in color at minimum light to < 0.016 magnitudes for the (r-i), (i-z), and (r-z) colors. These calibrations will be very useful for using RR Lyrae stars from DECam observations as both standard candles for distance determinations and color standards for reddening measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.03954v1-abstract-full').style.display = 'none'; document.getElementById('1707.03954v1-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 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </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 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/1701.00502">arXiv:1701.00502</a> <span> [<a href="https://arxiv.org/pdf/1701.00502">pdf</a>, <a href="https://arxiv.org/format/1701.00502">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/aa8d1c">10.3847/1538-3881/aa8d1c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SMASH - Survey of the MAgellanic Stellar History </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D+L">David L. Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">Knut Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+A+R">Alistair R. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Vivas%2C+A+K">A. Katherina Vivas</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Kaleida%2C+C">Catherine Kaleida</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+Y">Yumi Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Conn%2C+B+C">Blair C. Conn</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R+A">Robert A. Gruendl</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">Gurtina Besla</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=Gallart%2C+C">Carme Gallart</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Olszewski%2C+E+W">Edward W. Olszewski</a>, <a href="/search/astro-ph?searchtype=author&query=Saha%2C+A">Abhijit Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Monachesi%2C+A">Antonela Monachesi</a>, <a href="/search/astro-ph?searchtype=author&query=Monelli%2C+M">Matteo Monelli</a>, <a href="/search/astro-ph?searchtype=author&query=de+Boer%2C+T+J+L">Thomas J. L. de Boer</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+L+C">L. Clifton Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Zaritsky%2C+D">Dennis Zaritsky</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=van+der+Marel%2C+R+P">Roeland P. van der Marel</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=Jin%2C+S">Shoko Jin</a> , et al. (14 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="1701.00502v2-abstract-short" style="display: inline;"> The Large and Small Magellanic Clouds (LMC and SMC) are unique local laboratories for studying the formation and evolution of small galaxies in exquisite detail. The Survey of the MAgellanic Stellar History (SMASH) is an NOAO community DECam survey of the Clouds mapping 480 square degrees (distributed over ~2400 square degrees at ~20% filling factor) to ~24th mag in ugriz with the goal of identify… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.00502v2-abstract-full').style.display = 'inline'; document.getElementById('1701.00502v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1701.00502v2-abstract-full" style="display: none;"> The Large and Small Magellanic Clouds (LMC and SMC) are unique local laboratories for studying the formation and evolution of small galaxies in exquisite detail. The Survey of the MAgellanic Stellar History (SMASH) is an NOAO community DECam survey of the Clouds mapping 480 square degrees (distributed over ~2400 square degrees at ~20% filling factor) to ~24th mag in ugriz with the goal of identifying broadly distributed, low surface brightness stellar populations associated with the stellar halos and tidal debris of the Clouds. SMASH will also derive spatially-resolved star formation histories covering all ages out to large radii from the MCs that will further complement our understanding of their formation. Here, we present a summary of the survey, its data reduction, and a description of the first public Data Release (DR1). The SMASH DECam data have been reduced with a combination of the NOAO Community Pipeline, PHOTRED, an automated PSF photometry pipeline based mainly on the DAOPHOT suite, and custom calibration software. The attained astrometric precision is ~15 mas and the accuracy is ~2 mas with respect to the Gaia DR1 astrometric reference frame. The photometric precision is ~0.5-0.7% in griz and ~1% in u with a calibration accuracy of ~1.3% in all bands. The median 5 sigma point source depths in ugriz bands are 23.9, 24.8, 24.5, 24.2, 23.5 mag. The SMASH data already have been used to discover the Hydra II Milky Way satellite, the SMASH 1 old globular cluster likely associated with the LMC, and very extended stellar populations around the LMC out to R~18.4 kpc. SMASH DR1 contains measurements of ~100 million objects distributed in 61 fields. A prototype version of the NOAO Data Lab provides data access, including a data discovery tool, SMASH database access, an image cutout service, and a Jupyter notebook server with example notebooks for exploratory analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.00502v2-abstract-full').style.display = 'none'; document.getElementById('1701.00502v2-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2017. </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">23 pages, 12 figures. Revised and slightly reorganized based on referee's comments. 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/1611.00037">arXiv:1611.00037</a> <span> [<a href="https://arxiv.org/pdf/1611.00037">pdf</a>, <a href="https://arxiv.org/format/1611.00037">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The DESI Experiment Part II: Instrument Design </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aghamousa%2C+A">Amir Aghamousa</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">Jessica Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steve Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">Shadab Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+L+E">Lori E. Allen</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=Annis%2C+J">James Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">Stephen Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Balland%2C+C">Christophe Balland</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">Otger Ballester</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">Charles Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Beaufore%2C+L">Lucas Beaufore</a>, <a href="/search/astro-ph?searchtype=author&query=Bebek%2C+C">Chris Bebek</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=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Bernal%2C+J+L">Jos茅 Luis Bernal</a>, <a href="/search/astro-ph?searchtype=author&query=Besuner%2C+R">Robert Besuner</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">Florian Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">Chris Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Bleuler%2C+H">Hannes Bleuler</a>, <a href="/search/astro-ph?searchtype=author&query=Blomqvist%2C+M">Michael Blomqvist</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Bolton%2C+A+S">Adam S. Bolton</a>, <a href="/search/astro-ph?searchtype=author&query=Briceno%2C+C">Cesar Briceno</a> , et al. (268 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="1611.00037v2-abstract-short" style="display: inline;"> DESI (Dark Energy Spectropic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. The DESI instrument is a robotically-actuated, fiber-fed spectrograph capable of taking up to 5,000 simultaneous spectra over a wavelength range from… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00037v2-abstract-full').style.display = 'inline'; document.getElementById('1611.00037v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.00037v2-abstract-full" style="display: none;"> DESI (Dark Energy Spectropic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. The DESI instrument is a robotically-actuated, fiber-fed spectrograph capable of taking up to 5,000 simultaneous spectra over a wavelength range from 360 nm to 980 nm. The fibers feed ten three-arm spectrographs with resolution $R= 位/螖位$ between 2000 and 5500, depending on wavelength. The DESI instrument will be used to conduct a five-year survey designed to cover 14,000 deg$^2$. This powerful instrument will be installed at prime focus on the 4-m Mayall telescope in Kitt Peak, Arizona, along with a new optical corrector, which will provide a three-degree diameter field of view. The DESI collaboration will also deliver a spectroscopic pipeline and data management system to reduce and archive all data for eventual public use. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00037v2-abstract-full').style.display = 'none'; document.getElementById('1611.00037v2-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 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.00036">arXiv:1611.00036</a> <span> [<a href="https://arxiv.org/pdf/1611.00036">pdf</a>, <a href="https://arxiv.org/format/1611.00036">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The DESI Experiment Part I: Science,Targeting, and Survey Design </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DESI+Collaboration"> DESI Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aghamousa%2C+A">Amir Aghamousa</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">Jessica Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steve Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">Shadab Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+L+E">Lori E. Allen</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=Annis%2C+J">James Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">Stephen Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Balland%2C+C">Christophe Balland</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">Otger Ballester</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">Charles Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Beaufore%2C+L">Lucas Beaufore</a>, <a href="/search/astro-ph?searchtype=author&query=Bebek%2C+C">Chris Bebek</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=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Bernal%2C+J+L">Jos茅 Luis Bernal</a>, <a href="/search/astro-ph?searchtype=author&query=Besuner%2C+R">Robert Besuner</a>, <a href="/search/astro-ph?searchtype=author&query=Beutler%2C+F">Florian Beutler</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C">Chris Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Bleuler%2C+H">Hannes Bleuler</a>, <a href="/search/astro-ph?searchtype=author&query=Blomqvist%2C+M">Michael Blomqvist</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Bolton%2C+A+S">Adam S. Bolton</a>, <a href="/search/astro-ph?searchtype=author&query=Briceno%2C+C">Cesar Briceno</a> , et al. (268 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="1611.00036v2-abstract-short" style="display: inline;"> DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00036v2-abstract-full').style.display = 'inline'; document.getElementById('1611.00036v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.00036v2-abstract-full" style="display: none;"> DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure luminous red galaxies up to $z=1.0$. To probe the Universe out to even higher redshift, DESI will target bright [O II] emission line galaxies up to $z=1.7$. Quasars will be targeted both as direct tracers of the underlying dark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for the Ly-$伪$ forest absorption features in their spectra, which will be used to trace the distribution of neutral hydrogen. When moonlight prevents efficient observations of the faint targets of the baseline survey, DESI will conduct a magnitude-limited Bright Galaxy Survey comprising approximately 10 million galaxies with a median $z\approx 0.2$. In total, more than 30 million galaxy and quasar redshifts will be obtained to measure the BAO feature and determine the matter power spectrum, including redshift space distortions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00036v2-abstract-full').style.display = 'none'; document.getElementById('1611.00036v2-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 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.05918">arXiv:1609.05918</a> <span> [<a href="https://arxiv.org/pdf/1609.05918">pdf</a>, <a href="https://arxiv.org/ps/1609.05918">ps</a>, <a href="https://arxiv.org/format/1609.05918">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/10.3847/2041-8205/830/1/L10">10.3847/2041-8205/830/1/L10 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SMASH 1: a very faint globular cluster disrupting in the outer reaches of the LMC? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Jungbluth%2C+V">Valentin Jungbluth</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=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">Gurtina Besla</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</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=Conn%2C+B+C">Blair C. Conn</a>, <a href="/search/astro-ph?searchtype=author&query=Kaleida%2C+C+C">Catherine C. Kaleida</a>, <a href="/search/astro-ph?searchtype=author&query=Gallart%2C+C">Carme Gallart</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shoko Jin</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=Martinez-Delgado%2C+D">David Martinez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Monachesi%2C+A">Antonela Monachesi</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B1oz%2C+R+R">Ricardo R. M帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=No%C3%ABl%2C+N+E+D">Noelia E. D. No毛l</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">Knut Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Olszewski%2C+E+W">Edward W. Olszewski</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=van+der+Marel%2C+R+P">Roeland P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Vivas%2C+A+K">A. Katherina Vivas</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+A+R">Alistair R. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Zaritsky%2C+D">Dennis Zaritsky</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="1609.05918v2-abstract-short" style="display: inline;"> We present the discovery of a very faint stellar system, SMASH 1, that is potentially a satellite of the Large Magellanic Cloud. Found within the Survey of the MAgellanic Stellar History (SMASH), SMASH 1 is a compact ($r_h = 9.1^{+5.9}_{-3.4}$ pc) and very low luminosity (M_V = -1.0 +/- 0.9, $L_V=10^{2.3 +/- 0.4}$ Lsun) stellar system that is revealed by its sparsely populated main sequence and a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.05918v2-abstract-full').style.display = 'inline'; document.getElementById('1609.05918v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.05918v2-abstract-full" style="display: none;"> We present the discovery of a very faint stellar system, SMASH 1, that is potentially a satellite of the Large Magellanic Cloud. Found within the Survey of the MAgellanic Stellar History (SMASH), SMASH 1 is a compact ($r_h = 9.1^{+5.9}_{-3.4}$ pc) and very low luminosity (M_V = -1.0 +/- 0.9, $L_V=10^{2.3 +/- 0.4}$ Lsun) stellar system that is revealed by its sparsely populated main sequence and a handful of red-giant-branch candidate member stars. The photometric properties of these stars are compatible with a metal-poor ([Fe/H]=-2.2) and old (13 Gyr) isochrone located at a distance modulus of ~18.8, i.e. a distance of ~57 kpc. Situated at 11.3$^\circ$ from the LMC in projection, its 3-dimensional distance from the Cloud is ~13 kpc, consistent with a connection to the LMC, whose tidal radius is at least 16 kpc. Although the nature of SMASH 1 remains uncertain, its compactness favors it being a stellar cluster and hence dark-matter free. If this is the case, its dynamical tidal radius is only <19 pc at this distance from the LMC, and smaller than the system's extent on the sky. Its low luminosity and apparent high ellipticity ($蔚=0.62^{+0.17}_{-0.21}$) with its major axis pointing toward the LMC may well be the tell-tale sign of its imminent tidal demise. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.05918v2-abstract-full').style.display = 'none'; document.getElementById('1609.05918v2-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> 4 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </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, 4 figures, 1 table. Accepted for publication in ApJL. v2: corrected figure 4 in which rh for globular clusters were miscalculated. The updated figure reflect the published version of the paper</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.04639">arXiv:1607.04639</a> <span> [<a href="https://arxiv.org/pdf/1607.04639">pdf</a>, <a href="https://arxiv.org/format/1607.04639">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/10.1093/mnras/stw2122">10.1093/mnras/stw2122 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extinction law in the range 0.4-4.8 $渭$m and the 8620 $脜$ DIB towards the stellar cluster Westerlund 1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Damineli%2C+A">Augusto Damineli</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+L+A">Leonardo A. Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Damineli%2C+D+S+C">Daniel S. C. Damineli</a>, <a href="/search/astro-ph?searchtype=author&query=Navarete%2C+F">Felipe Navarete</a>, <a href="/search/astro-ph?searchtype=author&query=Rubinho%2C+M+S">Marcelo S. Rubinho</a>, <a href="/search/astro-ph?searchtype=author&query=Teodoro%2C+M">Mairan Teodoro</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="1607.04639v2-abstract-short" style="display: inline;"> The young stellar cluster Westerlund 1 (Wd 1: $l$=339.6$^\circ$, b=$-$0.4$^\circ$) is one of the most massive in the local Universe, but accurate parameters are pending on better determination of its extinction and distance. Based on our photometry and data collected from other sources, we have derived a reddening law for the cluster line-of-sight representative of the Galactic Plane (-5$^\circ<$b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.04639v2-abstract-full').style.display = 'inline'; document.getElementById('1607.04639v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.04639v2-abstract-full" style="display: none;"> The young stellar cluster Westerlund 1 (Wd 1: $l$=339.6$^\circ$, b=$-$0.4$^\circ$) is one of the most massive in the local Universe, but accurate parameters are pending on better determination of its extinction and distance. Based on our photometry and data collected from other sources, we have derived a reddening law for the cluster line-of-sight representative of the Galactic Plane (-5$^\circ<$b$<$+5$^\circ$) in the window 0.4-4.8 $渭$m: The power law exponent $伪$=2.13$\pm$0.08 is much steeper than those published a decade ago (1.6-1.8) and our index $R_V$=2.50$\pm$0.04 also differs from them, but in very good agreement with recent works based on deep surveys in the inner Galaxy. As a consequence, the total extinction $A_{Ks}$=0.74$ \pm $0.08 ($A_V$=11.40$ \pm$ 2.40) is substantially smaller than previous results(0.91-1.13), part of which ($A_{Ks}$=0.63 or $A_V$=9.66) is from the ISM. The extinction in front of the cluster spans a range of $螖A_V\sim$8.7\,mag with a gradient increasing from SW to NE across the cluster face, following the same general trend of warm dust distribution. The map of the $J-Ks$ colour index also shows a trend of reddening in this direction. We measured the equivalent width of the diffuse interstellar band at 8620 $脜$ (the "GAIA DIB") for Wd 1 cluster members and derived the relation $A_{Ks}$=0.612 $EW$ $-$ 0.191 $EW^2$. This extends the Munari et al. (2008) relation, valid for $E_{B-V}$ $<$ 1, to the non-linear regime ($A_V$ $>$ 4). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.04639v2-abstract-full').style.display = 'none'; document.getElementById('1607.04639v2-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 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2016. </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">to appear in MNRAS, 16 pages, 22 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/1606.03512">arXiv:1606.03512</a> <span> [<a href="https://arxiv.org/pdf/1606.03512">pdf</a>, <a href="https://arxiv.org/ps/1606.03512">ps</a>, <a href="https://arxiv.org/format/1606.03512">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/10.3847/0004-637X/825/1/54">10.3847/0004-637X/825/1/54 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mid Infrared View of the High Mass Star Formation Region W51A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barbosa%2C+C+L">Cassio L. Barbosa</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Damineli%2C+A">Augusto Damineli</a>, <a href="/search/astro-ph?searchtype=author&query=Conti%2C+P+S">Peter S. Conti</a>, <a href="/search/astro-ph?searchtype=author&query=Gusm%C3%A3o%2C+D+M">Danilo M. Gusm茫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="1606.03512v1-abstract-short" style="display: inline;"> In this paper we present the results of a mid infrared study of G49.5-0.4, or W51A, part of the massive starbirth complex W51. Combining public data from the $Spitzer$ IRAC camera, and Gemini mid infrared camera T-ReCS at 7.73, 9.69, 12.33 and 24.56 \micron, with spatial resolution of $\sim$0.5\arcsec, we have identified the mid infrared counterparts of 8 ultracompact HII regions, showing that two… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.03512v1-abstract-full').style.display = 'inline'; document.getElementById('1606.03512v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1606.03512v1-abstract-full" style="display: none;"> In this paper we present the results of a mid infrared study of G49.5-0.4, or W51A, part of the massive starbirth complex W51. Combining public data from the $Spitzer$ IRAC camera, and Gemini mid infrared camera T-ReCS at 7.73, 9.69, 12.33 and 24.56 \micron, with spatial resolution of $\sim$0.5\arcsec, we have identified the mid infrared counterparts of 8 ultracompact HII regions, showing that two radio sources are deeply embedded in molecular clouds and another is a cloud of ionized gas. From the T-ReCS data we have unveiled the central core of W51 region, revealing massive young stellar candidates. We modeled the spectral energy distribution of the detected sources suggesting the embedded objects are sources with spectral types ranging from B3 to O5, but the majority of the fits indicate stellar objects with B1 spectral types. We also present an extinction map of IRS~2, showing that a region with lower extinction corresponds to the region where a proposed jet of gas has impacted the foreground cloud. From this map, we also derived the total extinction towards the enigmatic source IRS~2E, which amounts to $\sim$60 magnitudes in the $V$ band. We calculated the color temperature due to thermal emission of the circumstellar dust of the detected sources; the temperatures are in the interval of $\sim$100 -- 150 K, which corresponds to the emission of dust located at 0.1 pc from the central source. Finally, we show a possible mid infrared counterpart of a detected source at mm wavelengths that was found by \cite{zap08,zap09} to be a massive young stellar object undergoing a high accretion rate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.03512v1-abstract-full').style.display = 'none'; document.getElementById('1606.03512v1-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, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2016. </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">42 pag, 9 fig. accepted by 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/1510.05539">arXiv:1510.05539</a> <span> [<a href="https://arxiv.org/pdf/1510.05539">pdf</a>, <a href="https://arxiv.org/ps/1510.05539">ps</a>, <a href="https://arxiv.org/format/1510.05539">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/10.3847/0004-6256/151/5/118">10.3847/0004-6256/151/5/118 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Variable stars in the field of the Hydra II ultra-faint dwarf galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vivas%2C+A+K">A. Katherina Vivas</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">Knut Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D">David Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+A">Alistair Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N">Nicolas Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">Gurtina Besla</a>, <a href="/search/astro-ph?searchtype=author&query=Gallart%2C+C">Carme Gallart</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R">Roeland van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S">Steven Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Kaleida%2C+C">Catherine Kaleida</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=Saha%2C+A">Abhijit Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Conn%2C+B">Blair Conn</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shoko Jin</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="1510.05539v2-abstract-short" style="display: inline;"> We report the discovery of one RR Lyrae star in the ultra--faint satellite galaxy Hydra II based on time series photometry in the g, r and i bands obtained with the Dark Energy Camera at Cerro Tololo Interamerican Observatory, Chile. The RR Lyrae star has a mean magnitude of $i = 21.30\pm 0.04$ which translates to a heliocentric distance of $151\pm 8$ kpc for Hydra II; this value is $\sim 13\%$ la… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.05539v2-abstract-full').style.display = 'inline'; document.getElementById('1510.05539v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.05539v2-abstract-full" style="display: none;"> We report the discovery of one RR Lyrae star in the ultra--faint satellite galaxy Hydra II based on time series photometry in the g, r and i bands obtained with the Dark Energy Camera at Cerro Tololo Interamerican Observatory, Chile. The RR Lyrae star has a mean magnitude of $i = 21.30\pm 0.04$ which translates to a heliocentric distance of $151\pm 8$ kpc for Hydra II; this value is $\sim 13\%$ larger than the estimate from the discovery paper based on the average magnitude of several blue horizontal branch star candidates. The new distance implies a slightly larger half-light radius of $76^{+12}_{-10}$ pc and a brighter absolute magnitude of $M_V = -5.1 \pm 0.3$, which keeps this object within the realm of the dwarf galaxies. The pulsational properties of the RR Lyrae star ($P=0.645$ d, $螖g = 0.68$ mag) suggest Hydra II may be a member of the intermediate Oosterhoff or Oosterhoff II group. A comparison with other RR Lyrae stars in ultra--faint systems indicates similar pulsational properties among them, which are different to those found among halo field stars and those in the largest of the Milky Way satellites. We also report the discovery of 31 additional short period variables in the field of view (RR Lyrae, SX Phe, eclipsing binaries, and a likely anomalous cepheid). However, given their magnitudes and large angular separation from Hydra II, they must be field stars not related to Hydra II. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.05539v2-abstract-full').style.display = 'none'; document.getElementById('1510.05539v2-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 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2015. </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">Revised version after comments from the referee. 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/1504.06174">arXiv:1504.06174</a> <span> [<a href="https://arxiv.org/pdf/1504.06174">pdf</a>, <a href="https://arxiv.org/format/1504.06174">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/10.1093/mnras/stv914">10.1093/mnras/stv914 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Survey of Extended H$_2$ Emission from Massive YSOs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Navarete%2C+F">Felipe Navarete</a>, <a href="/search/astro-ph?searchtype=author&query=Damineli%2C+A">Augusto Damineli</a>, <a href="/search/astro-ph?searchtype=author&query=Barbosa%2C+C+L">Cassio L. Barbosa</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">Robert D. Blum</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="1504.06174v1-abstract-short" style="display: inline;"> We present the results from a survey, designed to investigate the accretion process of massive young stellar objects (MYSOs) through near infrared narrow band imaging using the H$_2$ $谓$=1-0 S(1) transition filter. A sample of 353 Massive Young Stellar Object (MYSO) candidates was selected from the Red MSX Source survey using photometric criteria at longer wavelengths (infrared and submillimeter)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.06174v1-abstract-full').style.display = 'inline'; document.getElementById('1504.06174v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.06174v1-abstract-full" style="display: none;"> We present the results from a survey, designed to investigate the accretion process of massive young stellar objects (MYSOs) through near infrared narrow band imaging using the H$_2$ $谓$=1-0 S(1) transition filter. A sample of 353 Massive Young Stellar Object (MYSO) candidates was selected from the Red MSX Source survey using photometric criteria at longer wavelengths (infrared and submillimeter) and chosen with positions throughout the Galactic Plane. Our survey was carried out at the SOAR Telescope in Chile and CFHT in Hawaii covering both hemispheres. The data reveal that extended H$_2$ emission is a good tracer of outflow activity, which is a signpost of accretion process on young massive stars. Almost half of the sample exhibit extended H$_2$ emission and 74 sources (21\%) have polar morphology, suggesting collimated outflows. The polar-like structures are more likely to appear on radio-quiet sources, indicating these structures occur during the pre-UCHII phase. We also found an important fraction of sources associated with fluorescent H$_2$ diffuse emission that could be due to a more evolved phase. The images also indicate only $\sim$23\% (80) of the sample is associated with extant (young) stellar clusters. These results support the scenario in which massive stars are formed by accretion disks, since the merging of low mass stars would not produce outflow structures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.06174v1-abstract-full').style.display = 'none'; document.getElementById('1504.06174v1-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 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2015. </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">to appear on MNRAS. 18 pages, 86 figures and supplementary data available at CDS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.06216">arXiv:1503.06216</a> <span> [<a href="https://arxiv.org/pdf/1503.06216">pdf</a>, <a href="https://arxiv.org/ps/1503.06216">ps</a>, <a href="https://arxiv.org/format/1503.06216">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/10.1088/2041-8205/804/1/L5">10.1088/2041-8205/804/1/L5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hydra II: a faint and compact Milky Way dwarf galaxy found in the Survey of the Magellanic Stellar History </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</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=Besla%2C+G">Gurtina Besla</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">Knut Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+A+R">Alistair R. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Vivas%2C+A+K">A. Katherina Vivas</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R+A">Robert A. Gruendl</a>, <a href="/search/astro-ph?searchtype=author&query=Kaleida%2C+C+C">Catherine C. Kaleida</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=Blum%2C+R+D">Robert D. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Saha%2C+A">Abhijit Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Conn%2C+B+C">Blair C. Conn</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Chu%2C+Y">You-Hua Chu</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=de+Boer%2C+T+J+L">Thomas J. L. de Boer</a>, <a href="/search/astro-ph?searchtype=author&query=Gallart%2C+C">Carme Gallart</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shoko Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Kunder%2C+A">Andrea Kunder</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=Martinez-Delgado%2C+D">David Martinez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Monachesi%2C+A">Antonela Monachesi</a>, <a href="/search/astro-ph?searchtype=author&query=Monelli%2C+M">Matteo Monelli</a>, <a href="/search/astro-ph?searchtype=author&query=Monteagudo%2C+L">Lara Monteagudo</a>, <a href="/search/astro-ph?searchtype=author&query=No%C3%ABl%2C+N+E+D">Noelia E. D. No毛l</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="1503.06216v2-abstract-short" style="display: inline;"> We present the discovery of a new dwarf galaxy, Hydra II, found serendipitously within the data from the ongoing Survey of the MAgellanic Stellar History (SMASH) conducted with the Dark Energy Camera on the Blanco 4m Telescope. The new satellite is compact (r_h = 68 +/- 11 pc) and faint (M_V = -4.8 +/- 0.3), but well within the realm of dwarf galaxies. The stellar distribution of HydraII in the co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.06216v2-abstract-full').style.display = 'inline'; document.getElementById('1503.06216v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.06216v2-abstract-full" style="display: none;"> We present the discovery of a new dwarf galaxy, Hydra II, found serendipitously within the data from the ongoing Survey of the MAgellanic Stellar History (SMASH) conducted with the Dark Energy Camera on the Blanco 4m Telescope. The new satellite is compact (r_h = 68 +/- 11 pc) and faint (M_V = -4.8 +/- 0.3), but well within the realm of dwarf galaxies. The stellar distribution of HydraII in the color-magnitude diagram is well-described by a metal-poor ([Fe/H] = -2.2) and old (13 Gyr) isochrone and shows a distinct blue horizontal branch, some possible red clump stars, and faint stars that are suggestive of blue stragglers. At a heliocentric distance of 134 +/- 10 kpc, Hydra II is located in a region of the Galactic halo that models have suggested may host material from the leading arm of the Magellanic Stream. A comparison with N-body simulations hints that the new dwarf galaxy could be or could have been a satellite of the Magellanic Clouds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.06216v2-abstract-full').style.display = 'none'; document.getElementById('1503.06216v2-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 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2015. </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, 4 figures. Accepted for publication in ApJL. v2: minor corrections, conclusions unchanged</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.1067">arXiv:1408.1067</a> <span> [<a href="https://arxiv.org/pdf/1408.1067">pdf</a>, <a href="https://arxiv.org/ps/1408.1067">ps</a>, <a href="https://arxiv.org/format/1408.1067">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/10.1088/0004-6256/149/2/87">10.1088/0004-6256/149/2/87 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spitzer SAGE-Spec: Near Infrared Spectroscopy, Dust Shells, and Cool Envelopes in Extreme Large Magellanic Cloud AGB Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R+D">R. D. Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Srinivasan%2C+S">S. Srinivasan</a>, <a href="/search/astro-ph?searchtype=author&query=Kemper%2C+F">F. Kemper</a>, <a href="/search/astro-ph?searchtype=author&query=Ling%2C+B">B. Ling</a>, <a href="/search/astro-ph?searchtype=author&query=Volk%2C+K">K. Volk</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="1408.1067v1-abstract-short" style="display: inline;"> K-band spectra are presented for a sample of 39 Spitzer IRS SAGE-Spec sources in the Large Magellanic Cloud. The spectra exhibit characteristics in very good agreement with their positions in the near infrared - Spitzer color-magnitude diagrams and their properties as deduced from the Spitzer IRS spectra. Specifically, the near infrared spectra show strong atomic and molecular features representat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.1067v1-abstract-full').style.display = 'inline'; document.getElementById('1408.1067v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.1067v1-abstract-full" style="display: none;"> K-band spectra are presented for a sample of 39 Spitzer IRS SAGE-Spec sources in the Large Magellanic Cloud. The spectra exhibit characteristics in very good agreement with their positions in the near infrared - Spitzer color-magnitude diagrams and their properties as deduced from the Spitzer IRS spectra. Specifically, the near infrared spectra show strong atomic and molecular features representative of oxygen-rich and carbon-rich asymptotic giant branch stars, respectively. A small subset of stars were chosen from the luminous and red extreme "tip" of the color magnitude diagram. These objects have properties consistent with dusty envelopes but also cool, carbon-rich "stellar" cores. Modest amounts of dust mass loss combine with the stellar spectral energy distribution to make these objects appear extreme in their near infrared and mid infrared colors. One object in our sample, HV 915, a known post asymptotic giant branch star of the RV Tau type exhibits CO 2.3 micron band head emission consistent with previous work that demonstrates the object has a circumstellar disk. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.1067v1-abstract-full').style.display = 'none'; document.getElementById('1408.1067v1-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 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </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, 12 figures (eps), accepted for publication in the AJ</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" 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