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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/2410.06697">arXiv:2410.06697</a> <span> [<a href="https://arxiv.org/pdf/2410.06697">pdf</a>, <a href="https://arxiv.org/format/2410.06697">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> </div> </div> <p class="title is-5 mathjax"> JWST-IPA: Chemical Inventory and Spatial Mapping of Ices in the Protostar HOPS370 -- Evidence for an Opacity Hole and Thermal Processing of Ices </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tyagi%2C+H">Himanshu Tyagi</a>, <a href="/search/astro-ph?searchtype=author&query=P.%2C+M">Manoj P.</a>, <a href="/search/astro-ph?searchtype=author&query=Narang%2C+M">Mayank Narang</a>, <a href="/search/astro-ph?searchtype=author&query=Megeath%2C+S+T">S T. Megeath</a>, <a href="/search/astro-ph?searchtype=author&query=Rocha%2C+W+R+M">Will Robson M. Rocha</a>, <a href="/search/astro-ph?searchtype=author&query=Brunken%2C+N">Nashanty Brunken</a>, <a href="/search/astro-ph?searchtype=author&query=Rubinstein%2C+A+E">Adam E. Rubinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Gutermuth%2C+R+A">Robert A. Gutermuth</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+N+J">Neal J. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dishoeck%2C+E">Ewine van Dishoeck</a>, <a href="/search/astro-ph?searchtype=author&query=Federman%2C+S">Sam Federman</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+D+M">Dan M. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Neufeld%2C+D+A">David A. Neufeld</a>, <a href="/search/astro-ph?searchtype=author&query=Anglada%2C+G">Guillem Anglada</a>, <a href="/search/astro-ph?searchtype=author&query=Beuther%2C+H">Henrik Beuther</a>, <a href="/search/astro-ph?searchtype=author&query=Garatti%2C+A+C+o">Alessio Caratti o Garatti</a>, <a href="/search/astro-ph?searchtype=author&query=Looney%2C+L+W">Leslie W. Looney</a>, <a href="/search/astro-ph?searchtype=author&query=Nazari%2C+P">Pooneh Nazari</a>, <a href="/search/astro-ph?searchtype=author&query=Osorio%2C+M">Mayra Osorio</a>, <a href="/search/astro-ph?searchtype=author&query=Stanke%2C+T">Thomas Stanke</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+Y">Yao-Lun Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Bourke%2C+T+L">Tyler L. Bourke</a>, <a href="/search/astro-ph?searchtype=author&query=Fischer%2C+W+J">William J. Fischer</a>, <a href="/search/astro-ph?searchtype=author&query=Furlan%2C+E">Elise Furlan</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+J+D">Joel D. Green</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="2410.06697v1-abstract-short" style="display: inline;"> The composition of protoplanetary disks, and hence the initial conditions of planet formation, may be strongly influenced by the infall and thermal processing of material during the protostellar phase. Composition of dust and ice in protostellar envelopes, shaped by energetic processes driven by the protostar, serves as the fundamental building material for planets and complex organic molecules. A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.06697v1-abstract-full').style.display = 'inline'; document.getElementById('2410.06697v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.06697v1-abstract-full" style="display: none;"> The composition of protoplanetary disks, and hence the initial conditions of planet formation, may be strongly influenced by the infall and thermal processing of material during the protostellar phase. Composition of dust and ice in protostellar envelopes, shaped by energetic processes driven by the protostar, serves as the fundamental building material for planets and complex organic molecules. As part of the JWST GO program, "Investigating Protostellar Accretion" (IPA), we observed an intermediate-mass protostar HOPS 370 (OMC2-FIR3) using NIRSpec/IFU and MIRI/MRS. This study presents the gas and ice phase chemical inventory revealed with the JWST in the spectral range of $\sim$2.9 to 28 $渭$m and explores the spatial variation of volatile ice species in the protostellar envelope. We find evidence for thermal processing of ice species throughout the inner envelope. We present the first high-spatial resolution ($\sim 80$ au) maps of key volatile ice species H$_{2}$O, CO$_{2}$, $^{13}$CO$_2$, CO, and OCN$^-$, which reveal a highly structured and inhomogeneous density distribution of the protostellar envelope, with a deficiency of ice column density that coincides with the jet/outflow shocked knots. Further, we observe high relative crystallinity of H$_{2}$O ice around the shocked knot seen in the H$_2$ and OH wind/outflow, which can be explained by a lack of outer colder material in the envelope along the line of sight due to the irregular structure of the envelope. These observations show clear evidence of thermal processing of the ices in the inner envelope, close to the outflow cavity walls, heated by the luminous protostar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.06697v1-abstract-full').style.display = 'none'; document.getElementById('2410.06697v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Submitted to ApJ. Main text:16 pages with 11 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/2408.07974">arXiv:2408.07974</a> <span> [<a href="https://arxiv.org/pdf/2408.07974">pdf</a>, <a href="https://arxiv.org/format/2408.07974">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"> Unveiling the Cosmic Chemistry: Revisiting the Mass-Metallicity Relation with JWST/NIRSpec at 4 < z < 10 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sarkar%2C+A">Arnab Sarkar</a>, <a href="/search/astro-ph?searchtype=author&query=Chakraborty%2C+P">Priyanka Chakraborty</a>, <a href="/search/astro-ph?searchtype=author&query=Vogelsberger%2C+M">Mark Vogelsberger</a>, <a href="/search/astro-ph?searchtype=author&query=McDonald%2C+M">Michael McDonald</a>, <a href="/search/astro-ph?searchtype=author&query=Torrey%2C+P">Paul Torrey</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+A+M">Alex M. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Khullar%2C+G">Gourav Khullar</a>, <a href="/search/astro-ph?searchtype=author&query=Ferland%2C+G+J">Gary J. Ferland</a>, <a href="/search/astro-ph?searchtype=author&query=Forman%2C+W">William Forman</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">Scott Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+B">Benjamin Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Bautz%2C+M">Mark Bautz</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+E">Eric Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Grant%2C+C">Catherine Grant</a>, <a href="/search/astro-ph?searchtype=author&query=ZuHone%2C+J">John ZuHone</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="2408.07974v2-abstract-short" style="display: inline;"> We present star formation rates (SFR), the mass-metallicity relation (MZR), and the SFR-dependent MZR across redshifts 4 to 10 using 81 star-forming galaxies observed by the JWST NIRSpec employing both low-resolution PRISM and medium-resolution gratings, including galaxies from the JADES GOODS-N and GOODS-S fields, the JWST-PRIMAL Legacy Survey, and additional galaxies from the literature in Abell… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07974v2-abstract-full').style.display = 'inline'; document.getElementById('2408.07974v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.07974v2-abstract-full" style="display: none;"> We present star formation rates (SFR), the mass-metallicity relation (MZR), and the SFR-dependent MZR across redshifts 4 to 10 using 81 star-forming galaxies observed by the JWST NIRSpec employing both low-resolution PRISM and medium-resolution gratings, including galaxies from the JADES GOODS-N and GOODS-S fields, the JWST-PRIMAL Legacy Survey, and additional galaxies from the literature in Abell 2744, SMACS-0723, RXJ2129, BDF, COSMOS, and MACS1149 fields. These galaxies span a 3 dex stellar mass range of $10^7 < M_{\ast}/M_{\odot} < 10^{10}$, with an average SFR of $7.2 \pm 1.2 M_{\odot} {\rm yr}^{-1}$ and an average metallicity of $12+{\rm log(O/H)} = 7.91 \pm 0.08$. Our findings align with previous observations up to $z=8$ for the MZR and indicate no deviation from local universe FMR up to this redshift. Beyond $z=8$, we observe a significant deviation $\sim 0.27$ dex) in FMR, consistent with recent JWST findings. We also integrate CEERS (135 galaxies) and JADES (47 galaxies) samples with our data to study metallicity evolution with redshift in a combined sample of 263 galaxies, revealing a decreasing metallicity trend with a slope of $0.067 \pm 0.013$, consistent with IllustrisTNG and EAGLE, but contradicts with FIRE simulations. We introduce an empirical mass-metallicity-redshift (MZ-$z$ relation): $12+{\rm log(O/H)}=6.29 + 0.237 \times{\rm log}(M_{\ast}/M_{\odot}) - 0.06 \times (1+z)$, which accurately reproduces the observed trends in metallicity with both redshift and stellar mass. This trend underscores the ``Grand Challenge'' in understanding the factors driving high-redshift galactic metallicity trends, such as inflow, outflow, and AGN/stellar feedback -- and emphasizes the need for further investigations with larger samples and enhanced simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07974v2-abstract-full').style.display = 'none'; document.getElementById('2408.07974v2-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">24 Pages, 9 Figures. Submitted to ApJ. Comments are 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/2406.05306">arXiv:2406.05306</a> <span> [<a href="https://arxiv.org/pdf/2406.05306">pdf</a>, <a href="https://arxiv.org/format/2406.05306">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"> Detection of New Galaxy Candidates at $z\ >$ 11 in the JADES Field Using JWST NIRCam </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chakraborty%2C+P">Priyanka Chakraborty</a>, <a href="/search/astro-ph?searchtype=author&query=Sarkar%2C+A">Arnab Sarkar</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">Scott Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+B">Benjamin Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Brickhouse%2C+N">Nancy Brickhouse</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzetta%2C+K">Kenneth Lanzetta</a>, <a href="/search/astro-ph?searchtype=author&query=Foster%2C+A">Adam Foster</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R">Randall Smith</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.05306v2-abstract-short" style="display: inline;"> We report the detection of seven new galaxy candidates with redshift $z$ $>$ 11 within the JWST Advanced Deep Extragalactic Survey (JADES) GOODS-S and GOODS-N fields. These new candidates are detected through meticulous analysis of NIRCam photometry in eight filters spanning a wavelength range of 0.8-5.0 $渭$m. Photometric redshifts of these galaxy candidates are independently measured utilizing sp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05306v2-abstract-full').style.display = 'inline'; document.getElementById('2406.05306v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05306v2-abstract-full" style="display: none;"> We report the detection of seven new galaxy candidates with redshift $z$ $>$ 11 within the JWST Advanced Deep Extragalactic Survey (JADES) GOODS-S and GOODS-N fields. These new candidates are detected through meticulous analysis of NIRCam photometry in eight filters spanning a wavelength range of 0.8-5.0 $渭$m. Photometric redshifts of these galaxy candidates are independently measured utilizing spectral energy distribution (SED) fitting techniques using \texttt{EAZY} and \texttt{BAGPIPES} codes, followed by visual scrutiny. Two of these galaxy candidates are located in GOODS-S field, while the remaining five galaxies are located in GOODS-N field. Our analysis reveals that the stellar masses of these galaxies typically range from log $M_{\ast}$/$M_{\odot}$ = 7.75--8.75. Futhermore, these galaxies are typically young with their mass-weighted ages spanning from 80 to 240 Myr. Their specific star formation rates (sSFR), quantified as $\log (\text{sSFR}/\text{Gyr}$), are measured to vary between $\sim 0.95$ to 1.46. These new galaxy candidates offer a robust sample for probing the physical properties of galaxies within the first few hundred Myr of the history of the Universe. We also analyze the relationship between star formation rate (SFR) and stellar mass ($M_\ast$) within our sample. Using linear regression, our analysis yields a slope of $0.71 \pm 0.12$, which we then compare with results from previous studies. Continued investigation through spectroscopic analysis using JWST/NIRSpec is needed to spectroscopically confirm these high-redshift galaxy candidates and investigate further into their physical properties. We plan to follow up on these candidates with future NIRSpec observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05306v2-abstract-full').style.display = 'none'; document.getElementById('2406.05306v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 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/2404.07299">arXiv:2404.07299</a> <span> [<a href="https://arxiv.org/pdf/2404.07299">pdf</a>, <a href="https://arxiv.org/ps/2404.07299">ps</a>, <a href="https://arxiv.org/format/2404.07299">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"> JWST/MIRI detection of suprathermal OH rotational emissions: probing the dissociation of the water by Lyman alpha photons near the protostar HOPS 370 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Neufeld%2C+D+A">David A. Neufeld</a>, <a href="/search/astro-ph?searchtype=author&query=Manoj%2C+P">P. Manoj</a>, <a href="/search/astro-ph?searchtype=author&query=Tyagi%2C+H">Himanshu Tyagi</a>, <a href="/search/astro-ph?searchtype=author&query=Narang%2C+M">Mayank Narang</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+D+M">Dan M. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Megeath%2C+S+T">S. Thomas Megeath</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Dishoeck%2C+E+F">Ewine F. Van Dishoeck</a>, <a href="/search/astro-ph?searchtype=author&query=Gutermuth%2C+R+A">Robert A. Gutermuth</a>, <a href="/search/astro-ph?searchtype=author&query=Stanke%2C+T">Thomas Stanke</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+Y">Yao-Lun Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Rubinstein%2C+A+E">Adam E. Rubinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Anglada%2C+G">Guillem Anglada</a>, <a href="/search/astro-ph?searchtype=author&query=Beuther%2C+H">Henrik Beuther</a>, <a href="/search/astro-ph?searchtype=author&query=Garatti%2C+A+C+o">Alessio Caratti o Garatti</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+N+J">Neal J. Evans II</a>, <a href="/search/astro-ph?searchtype=author&query=Federman%2C+S">Samuel Federman</a>, <a href="/search/astro-ph?searchtype=author&query=Fischer%2C+W+J">William J. Fischer</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+J">Joel Green</a>, <a href="/search/astro-ph?searchtype=author&query=Klaassen%2C+P">Pamela Klaassen</a>, <a href="/search/astro-ph?searchtype=author&query=Looney%2C+L+W">Leslie W. Looney</a>, <a href="/search/astro-ph?searchtype=author&query=Osorio%2C+M">Mayra Osorio</a>, <a href="/search/astro-ph?searchtype=author&query=Nazari%2C+P">Pooneh Nazari</a>, <a href="/search/astro-ph?searchtype=author&query=Tobin%2C+J+J">John J. Tobin</a>, <a href="/search/astro-ph?searchtype=author&query=Tychoniec%2C+L">Lukasz Tychoniec</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">Scott Wolk</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.07299v1-abstract-short" style="display: inline;"> Using the MIRI/MRS spectrometer on JWST, we have detected pure rotational, suprathermal OH emissions from the vicinity of the intermediate-mass protostar HOPS 370 (OMC2/FIR3). These emissions are observed from shocked knots in a jet/outflow, and originate in states of rotational quantum number as high as 46 that possess excitation energies as large as $E_U/k = 4.65 \times 10^4$ K. The relative str… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07299v1-abstract-full').style.display = 'inline'; document.getElementById('2404.07299v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.07299v1-abstract-full" style="display: none;"> Using the MIRI/MRS spectrometer on JWST, we have detected pure rotational, suprathermal OH emissions from the vicinity of the intermediate-mass protostar HOPS 370 (OMC2/FIR3). These emissions are observed from shocked knots in a jet/outflow, and originate in states of rotational quantum number as high as 46 that possess excitation energies as large as $E_U/k = 4.65 \times 10^4$ K. The relative strengths of the observed OH lines provide a powerful diagnostic of the ultraviolet radiation field in a heavily-extinguished region ($A_V \sim 10 - 20$) where direct UV observations are impossible. To high precision, the OH line strengths are consistent with a picture in which the suprathermal OH states are populated following the photodissociation of water in its $\tilde B - X$ band by ultraviolet radiation produced by fast ($\sim 80\,\rm km\,s^{-1}$) shocks along the jet. The observed dominance of emission from symmetric ($A^\prime$) OH states over that from antisymmetric ($A^{\prime\prime}$) states provides a distinctive signature of this particular population mechanism. Moreover, the variation of intensity with rotational quantum number suggests specifically that Ly$伪$ radiation is responsible for the photodissociation of water, an alternative model with photodissociation by a 10$^4$ K blackbody being disfavored at a high level of significance. Using measurements of the Br$伪$ flux to estimate the Ly$伪$ production rate, we find that $\sim 4\%$ of the Ly$伪$ photons are absorbed by water. Combined with direct measurements of water emissions in the $谓_2 = 1 -0$ band, the OH observations promise to provide key constraints on future models for the diffusion of Ly$伪$ photons in the vicinity of a shock front. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07299v1-abstract-full').style.display = 'none'; document.getElementById('2404.07299v1-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 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">30 pages, 7 figures. Accepted for publication in ApJ Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.04314">arXiv:2402.04314</a> <span> [<a href="https://arxiv.org/pdf/2402.04314">pdf</a>, <a href="https://arxiv.org/format/2402.04314">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202348718">10.1051/0004-6361/202348718 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JWST observations of $^{13}$CO$_{2}$ ice: Tracing the chemical environment and thermal history of ices in protostellar envelopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brunken%2C+N+G+C">Nashanty G. C. Brunken</a>, <a href="/search/astro-ph?searchtype=author&query=Rocha%2C+W+R+M">Will R. M. Rocha</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dishoeck%2C+E+F">Ewine F. van Dishoeck</a>, <a href="/search/astro-ph?searchtype=author&query=Gutermuth%2C+R">Robert Gutermuth</a>, <a href="/search/astro-ph?searchtype=author&query=Tyagi%2C+H">Himanshu Tyagi</a>, <a href="/search/astro-ph?searchtype=author&query=Slavicinska%2C+K">Katerina Slavicinska</a>, <a href="/search/astro-ph?searchtype=author&query=Nazari%2C+P">Pooneh Nazari</a>, <a href="/search/astro-ph?searchtype=author&query=Megeath%2C+S+T">S. Thomas Megeath</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+N+J">Neal J. Evans II</a>, <a href="/search/astro-ph?searchtype=author&query=Narang%2C+M">Mayank Narang</a>, <a href="/search/astro-ph?searchtype=author&query=Manoj%2C+P">P. Manoj</a>, <a href="/search/astro-ph?searchtype=author&query=Rubinstein%2C+A+E">Adam E. Rubinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+D+M">Dan M. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Looney%2C+L+W">Leslie W. Looney</a>, <a href="/search/astro-ph?searchtype=author&query=Linnartz%2C+H">Harold Linnartz</a>, <a href="/search/astro-ph?searchtype=author&query=Garatti%2C+A+C+o">Alessio Caratti o Garatti</a>, <a href="/search/astro-ph?searchtype=author&query=Beuther%2C+H">Henrik Beuther</a>, <a href="/search/astro-ph?searchtype=author&query=Linz%2C+H">Hendrik Linz</a>, <a href="/search/astro-ph?searchtype=author&query=Klaassen%2C+P">Pamela Klaassen</a>, <a href="/search/astro-ph?searchtype=author&query=Poteet%2C+C+A">Charles A. Poteet</a>, <a href="/search/astro-ph?searchtype=author&query=Federman%2C+S">Samuel Federman</a>, <a href="/search/astro-ph?searchtype=author&query=Anglada%2C+G">Guillem Anglada</a>, <a href="/search/astro-ph?searchtype=author&query=Atnagulov%2C+P">Prabhani Atnagulov</a>, <a href="/search/astro-ph?searchtype=author&query=Bourke%2C+T+L">Tyler L. Bourke</a>, <a href="/search/astro-ph?searchtype=author&query=Fischer%2C+W+J">William J. Fischer</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="2402.04314v2-abstract-short" style="display: inline;"> The structure and composition of simple ices can be modified during stellar evolution by protostellar heating. Key to understanding the involved processes are thermal and chemical tracers that can diagnose the history and environment of the ice. The 15.2 $渭$m bending mode of $^{12}$CO$_2$ has proven to be a valuable tracer of ice heating events but suffers from grain shape and size effects. A viab… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.04314v2-abstract-full').style.display = 'inline'; document.getElementById('2402.04314v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.04314v2-abstract-full" style="display: none;"> The structure and composition of simple ices can be modified during stellar evolution by protostellar heating. Key to understanding the involved processes are thermal and chemical tracers that can diagnose the history and environment of the ice. The 15.2 $渭$m bending mode of $^{12}$CO$_2$ has proven to be a valuable tracer of ice heating events but suffers from grain shape and size effects. A viable alternative tracer is the weaker $^{13}$CO$_2$ isotopologue band at 4.39 $渭$m which has now become accessible at high S/N with the $\textit{James Webb}$ Space Telescope (JWST). We present JWST NIRSpec observations of $^{13}$CO$_2$ ice in five deeply embedded Class 0 sources spanning a wide range in luminosities (0.2 - 10$^4$ L$_{\odot}$ ) taken as part of the Investigating Protostellar Accretion Across the Mass Spectrum (IPA) program. The band profiles vary significantly, with the most luminous sources showing a distinct narrow peak at 4.38 $渭$m. We first apply a phenomenological approach and show that a minimum of 3-4 Gaussian profiles are needed to fit the $^{13}$CO$_2$ absorption feature. We then combine these findings with laboratory data and show that a 15.2 $渭$m $^{12}$CO$_2$ band inspired five-component decomposition can be applied for the isotopologue band where each component is representative of CO$_2$ ice in a specific molecular environment. The final solution consists of cold mixtures of CO$_2$ with CH$_3$OH, H$_2$O and CO as well as segregated heated pure CO$_2$ ice. Our results are in agreement with previous studies of the $^{12}$CO$_2$ ice band, further confirming that $^{13}$CO$_{2}$ is a useful alternative tracer of protostellar heating events. We also propose an alternative solution consisting only of heated CO$_2$:CH$_3$OH and CO$_2$:H$_2$O ices and warm pure CO$_2$ ice for decomposing the ice profiles of the two most luminous sources in our sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.04314v2-abstract-full').style.display = 'none'; document.getElementById('2402.04314v2-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 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">Journal ref:</span> A&A 685, A27 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.01932">arXiv:2401.01932</a> <span> [<a href="https://arxiv.org/pdf/2401.01932">pdf</a>, <a href="https://arxiv.org/format/2401.01932">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> ABYSS II: Identification of young stars in optical SDSS spectra and their properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saad%2C+S">Serat Saad</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+K">Kaitlyn Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Kounkel%2C+M">Marina Kounkel</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Valdivia%2C+R">Ricardo L贸pez-Valdivia</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J+S">Jinyoung Serena Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez%2C+K+P">Karla Pe帽a Ram铆rez</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=Rom%C3%A1n-Z%C3%BA%C3%B1iga%2C+C+G">Carlos G. Rom谩n-Z煤帽iga</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">Jes煤s Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Hillenbrand%2C+L+A">Lynne A. Hillenbrand</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="2401.01932v1-abstract-short" style="display: inline;"> We developed a tool that measures equivalent widths of various lines in low resolution optical spectra, and it was applied to stellar spectra obtained as part of SDSS-V and LAMOST programs. These lines, such as Li I which directly indicates stellar youth, or optical H I and Ca II which in emission indicate activity associated with stellar youth, are commonly seen in YSOs. We observe several notabl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.01932v1-abstract-full').style.display = 'inline'; document.getElementById('2401.01932v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.01932v1-abstract-full" style="display: none;"> We developed a tool that measures equivalent widths of various lines in low resolution optical spectra, and it was applied to stellar spectra obtained as part of SDSS-V and LAMOST programs. These lines, such as Li I which directly indicates stellar youth, or optical H I and Ca II which in emission indicate activity associated with stellar youth, are commonly seen in YSOs. We observe several notable differences in the properties of these lines between YSOs and the field stars. Using these data, we devise a set of criteria through which it is possible to confirm the youth of stars that have been observed by the ABYSS program, as well as to identify likely young stars that have serendipitously been observed by other programs. We examine the decrement of H lines seen in emission in CTTSs, and estimate the properties of the accretion stream that is responsible for the production of these lines. Finally, we examine the evolution of Li I as a function of age, and characterize the scatter in its abundance that appears to be intrinsic in young M dwarfs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.01932v1-abstract-full').style.display = 'none'; document.getElementById('2401.01932v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">15 pages, 10 figures, accepted to AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.07807">arXiv:2312.07807</a> <span> [<a href="https://arxiv.org/pdf/2312.07807">pdf</a>, <a href="https://arxiv.org/format/2312.07807">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> IPA: Class 0 Protostars Viewed in CO Emission Using JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rubinstein%2C+A+E">Adam E. Rubinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+N+J">Neal J. Evans II</a>, <a href="/search/astro-ph?searchtype=author&query=Tyagi%2C+H">Himanshu Tyagi</a>, <a href="/search/astro-ph?searchtype=author&query=Narang%2C+M">Mayank Narang</a>, <a href="/search/astro-ph?searchtype=author&query=Nazari%2C+P">Pooneh Nazari</a>, <a href="/search/astro-ph?searchtype=author&query=Gutermuth%2C+R">Robert Gutermuth</a>, <a href="/search/astro-ph?searchtype=author&query=Federman%2C+S">Samuel Federman</a>, <a href="/search/astro-ph?searchtype=author&query=Manoj%2C+P">P. Manoj</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+J+D">Joel D. Green</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+D+M">Dan M. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Megeath%2C+S+T">S. Thomas Megeath</a>, <a href="/search/astro-ph?searchtype=author&query=Rocha%2C+W+R+M">Will R. M. Rocha</a>, <a href="/search/astro-ph?searchtype=author&query=Brunken%2C+N+G+C">Nashanty G. C. Brunken</a>, <a href="/search/astro-ph?searchtype=author&query=Slavicinska%2C+K">Katerina Slavicinska</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dishoeck%2C+E+F">Ewine F. van Dishoeck</a>, <a href="/search/astro-ph?searchtype=author&query=Beuther%2C+H">Henrik Beuther</a>, <a href="/search/astro-ph?searchtype=author&query=Bourke%2C+T+L">Tyler L. Bourke</a>, <a href="/search/astro-ph?searchtype=author&query=Garatti%2C+A+C+o">Alessio Caratti o Garatti</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+L">Lee Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=Klaassen%2C+P">Pamela Klaassen</a>, <a href="/search/astro-ph?searchtype=author&query=Linz%2C+H">Hendrik Linz</a>, <a href="/search/astro-ph?searchtype=author&query=Looney%2C+L+W">Leslie W. Looney</a>, <a href="/search/astro-ph?searchtype=author&query=Muzerolle%2C+J">James Muzerolle</a>, <a href="/search/astro-ph?searchtype=author&query=Stanke%2C+T">Thomas Stanke</a>, <a href="/search/astro-ph?searchtype=author&query=Tobin%2C+J+J">John J. Tobin</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="2312.07807v2-abstract-short" style="display: inline;"> We investigate the bright CO fundamental emission in the central regions of five protostars in their primary mass assembly phase using new observations from JWST's Near-Infrared Spectrograph (NIRSpec) and Mid-Infrared Instrument (MIRI). CO line emission images and fluxes are extracted for a forest of $\sim$150 ro-vibrational transitions from two vibrational bands, $v=1-0$ and $v=2-1$. However,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07807v2-abstract-full').style.display = 'inline'; document.getElementById('2312.07807v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.07807v2-abstract-full" style="display: none;"> We investigate the bright CO fundamental emission in the central regions of five protostars in their primary mass assembly phase using new observations from JWST's Near-Infrared Spectrograph (NIRSpec) and Mid-Infrared Instrument (MIRI). CO line emission images and fluxes are extracted for a forest of $\sim$150 ro-vibrational transitions from two vibrational bands, $v=1-0$ and $v=2-1$. However, ${}^{13}$CO is undetected, indicating that ${}^{12}$CO emission is optically thin. We use H$_2$ emission lines to correct fluxes for extinction and then construct rotation diagrams for the CO lines with the highest spectral resolution and sensitivity to estimate rotational temperatures and numbers of CO molecules. Two distinct rotational temperature components are required for $v=1$ ($\sim600$ to 1000 K and 2000 to $\sim 10^4$ K), while one hotter component is required for $v=2$ ($\gtrsim 3500$ K). ${}^{13}$CO is depleted compared to the abundances found in the ISM, indicating selective UV photodissociation of ${}^{13}$CO; therefore, UV radiative pumping may explain the higher rotational temperatures in $v=2$. The average vibrational temperature is $\sim 1000$ K for our sources and is similar to the lowest rotational temperature components. Using the measured rotational and vibrational temperatures to infer a total number of CO molecules, we find that the total gas masses range from lower limits of $\sim10^{22}$ g for the lowest mass protostars to $\sim 10^{26}$ g for the highest mass protostars. Our gas mass lower limits are compatible with those in more evolved systems, which suggest the lowest rotational temperature component comes from the inner disk, scattered into our line of sight, but we also cannot exclude the contribution to the CO emission from disk winds for higher mass targets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07807v2-abstract-full').style.display = 'none'; document.getElementById('2312.07807v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">31 pages, 7 figures, 4 tables, received to ApJ December 10 2023, accepted to ApJ August 4 2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.07674">arXiv:2311.07674</a> <span> [<a href="https://arxiv.org/pdf/2311.07674">pdf</a>, <a href="https://arxiv.org/format/2311.07674">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="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The life cycle of stars and their planets from the high energy perspective </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Corrales%2C+L">Lia Corrales</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Cunningham%2C+T">Tim Cunningham</a>, <a href="/search/astro-ph?searchtype=author&query=Duvvuri%2C+G">Girish Duvvuri</a>, <a href="/search/astro-ph?searchtype=author&query=Drake%2C+J+J">Jeremy J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Espaillat%2C+C">Catherine Espaillat</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+A+D">Adina D. Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Gallo%2C+E">Elena Gallo</a>, <a href="/search/astro-ph?searchtype=author&query=Gunther%2C+H+M">Hans Moritz Gunther</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+G+W">George W. King</a>, <a href="/search/astro-ph?searchtype=author&query=Kounkel%2C+M">Marina Kounkel</a>, <a href="/search/astro-ph?searchtype=author&query=Lisse%2C+C+M">Carey M. Lisse</a>, <a href="/search/astro-ph?searchtype=author&query=Montez%2C+R">Rodolfo Montez Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Principe%2C+D+A">David A. Principe</a>, <a href="/search/astro-ph?searchtype=author&query=Toala%2C+J+A">Jesus A. Toala</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Cilley%2C+R">Raven Cilley</a>, <a href="/search/astro-ph?searchtype=author&query=Daylan%2C+T">Tansu Daylan</a>, <a href="/search/astro-ph?searchtype=author&query=Karovska%2C+M">Margarita Karovska</a>, <a href="/search/astro-ph?searchtype=author&query=Pradhan%2C+P">Pragati Pradhan</a>, <a href="/search/astro-ph?searchtype=author&query=Wheatley%2C+P+J">Peter J. Wheatley</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+J">Jun Yang</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="2311.07674v1-abstract-short" style="display: inline;"> One of the key research themes identified by the Astro2020 decadal survey is Worlds and Suns in Context. The Advanced X-ray Imaging Satellite (AXIS) is a proposed NASA APEX mission that will become the prime high-energy instrument for studying star-planet connections from birth to death. This work explores the major advances in this broad domain of research that will be enabled by the AXIS mission… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.07674v1-abstract-full').style.display = 'inline'; document.getElementById('2311.07674v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.07674v1-abstract-full" style="display: none;"> One of the key research themes identified by the Astro2020 decadal survey is Worlds and Suns in Context. The Advanced X-ray Imaging Satellite (AXIS) is a proposed NASA APEX mission that will become the prime high-energy instrument for studying star-planet connections from birth to death. This work explores the major advances in this broad domain of research that will be enabled by the AXIS mission, through X-ray observations of stars in clusters spanning a broad range of ages, flaring M-dwarf stars known to host exoplanets, and young stars exhibiting accretion interactions with their protoplanetary disks. In addition, we explore the ability of AXIS to use planetary nebulae, white dwarfs, and the Solar System to constrain important physical processes from the microscopic (e.g., charge exchange) to the macroscopic (e.g., stellar wind interactions with the surrounding interstellar medium). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.07674v1-abstract-full').style.display = 'none'; document.getElementById('2311.07674v1-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 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">This White Paper is part of a series commissioned for the AXIS Probe Concept Mission</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.14061">arXiv:2310.14061</a> <span> [<a href="https://arxiv.org/pdf/2310.14061">pdf</a>, <a href="https://arxiv.org/format/2310.14061">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Discovery of a collimated jet from the low luminosity protostar IRAS 16253$-$2429 in a quiescent accretion phase with the JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Narang%2C+M">Mayank Narang</a>, <a href="/search/astro-ph?searchtype=author&query=P.%2C+M">Manoj P.</a>, <a href="/search/astro-ph?searchtype=author&query=Tyagi%2C+H">Himanshu Tyagi</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+D+M">Dan M. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Megeath%2C+S+T">S. Thomas Megeath</a>, <a href="/search/astro-ph?searchtype=author&query=Federman%2C+S">Samuel Federman</a>, <a href="/search/astro-ph?searchtype=author&query=Rubinstein%2C+A+E">Adam E. Rubinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Gutermuth%2C+R">Robert Gutermuth</a>, <a href="/search/astro-ph?searchtype=author&query=Garatti%2C+A+C+o">Alessio Caratti o Garatti</a>, <a href="/search/astro-ph?searchtype=author&query=Beuther%2C+H">Henrik Beuther</a>, <a href="/search/astro-ph?searchtype=author&query=Bourke%2C+T+L">Tyler L. Bourke</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Dishoeck%2C+E+F">Ewine F. Van Dishoeck</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+N+J">Neal J. Evans II</a>, <a href="/search/astro-ph?searchtype=author&query=Anglada%2C+G">Guillem Anglada</a>, <a href="/search/astro-ph?searchtype=author&query=Osorio%2C+M">Mayra Osorio</a>, <a href="/search/astro-ph?searchtype=author&query=Stanke%2C+T">Thomas Stanke</a>, <a href="/search/astro-ph?searchtype=author&query=Muzerolle%2C+J">James Muzerolle</a>, <a href="/search/astro-ph?searchtype=author&query=Looney%2C+L+W">Leslie W. Looney</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+Y">Yao-Lun Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Tobin%2C+J+J">John J. Tobin</a>, <a href="/search/astro-ph?searchtype=author&query=Klaassen%2C+P">Pamela Klaassen</a>, <a href="/search/astro-ph?searchtype=author&query=Karnath%2C+N">Nicole Karnath</a>, <a href="/search/astro-ph?searchtype=author&query=Atnagulov%2C+P">Prabhani Atnagulov</a>, <a href="/search/astro-ph?searchtype=author&query=Brunken%2C+N">Nashanty Brunken</a>, <a href="/search/astro-ph?searchtype=author&query=Fischer%2C+W+J">William J. Fischer</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="2310.14061v5-abstract-short" style="display: inline;"> Investigating Protostellar Accretion (IPA) is a JWST Cycle~1 GO program that uses NIRSpec IFU and MIRI MRS to obtain 2.9--28~$渭$m spectral cubes of young, deeply embedded protostars with luminosities of 0.2 to 10,000~L$_{\odot}$ and central masses of 0.15 to 12~M$_{\odot}$. In this Letter, we report the discovery of a highly collimated atomic jet from the Class~0 protostar IRAS~16253$-$2429, the l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.14061v5-abstract-full').style.display = 'inline'; document.getElementById('2310.14061v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.14061v5-abstract-full" style="display: none;"> Investigating Protostellar Accretion (IPA) is a JWST Cycle~1 GO program that uses NIRSpec IFU and MIRI MRS to obtain 2.9--28~$渭$m spectral cubes of young, deeply embedded protostars with luminosities of 0.2 to 10,000~L$_{\odot}$ and central masses of 0.15 to 12~M$_{\odot}$. In this Letter, we report the discovery of a highly collimated atomic jet from the Class~0 protostar IRAS~16253$-$2429, the lowest luminosity source ($L_\mathrm{bol}$ = 0.2 $L_\odot$) in the IPA program. The collimated jet is detected in multiple [Fe~II] lines, [Ne~II], [Ni~II], and H~I lines, but not in molecular emission. The atomic jet has a velocity of about 169~$\pm$~15~km\,s$^{-1}$, after correcting for inclination. The width of the jet increases with distance from the central protostar from 23 to~60 au, corresponding to an opening angle of 2.6~$\pm$~0.5\arcdeg. By comparing the measured flux ratios of various fine structure lines to those predicted by simple shock models, we derive a shock {speed} of 54~km\,s$^{-1}$ and a preshock density of 2.0$\times10^{3}$~cm$^{-3}$ at the base of the jet. {From these quantities and using a suite of jet models and extinction laws we compute a mass loss rate between $0.4 -1.1\times10^{-10}~M_{\odot}$~yr~$^{-1}$.} The low mass loss rate is consistent with simultaneous measurements of low mass accretion rate ($2.4~\pm~0.8~\times~10^{-9}~M_{\odot}$~yr$^{-1}$) for IRAS~16253$-$2429 from JWST observations (Watson et al. in prep), indicating that the protostar is in a quiescent accretion phase. Our results demonstrate that very low-mass protostars can drive highly collimated, atomic jets, even during the quiescent phase. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.14061v5-abstract-full').style.display = 'none'; document.getElementById('2310.14061v5-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">Accepted to ApJL. Comments and feedback 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/2310.13873">arXiv:2310.13873</a> <span> [<a href="https://arxiv.org/pdf/2310.13873">pdf</a>, <a href="https://arxiv.org/format/2310.13873">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="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Revolutionary Solar System Science Enabled by the Line Emission Mapper X-ray Probe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+W+R">William R. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Koutroumpa%2C+D">Dimitra Koutroumpa</a>, <a href="/search/astro-ph?searchtype=author&query=Carter%2C+J+A">Jennifer A. Carter</a>, <a href="/search/astro-ph?searchtype=author&query=Kuntz%2C+K+D">Kip D. Kuntz</a>, <a href="/search/astro-ph?searchtype=author&query=McEntee%2C+S">Sean McEntee</a>, <a href="/search/astro-ph?searchtype=author&query=Deskins%2C+T">Thomas Deskins</a>, <a href="/search/astro-ph?searchtype=author&query=Parry%2C+B">Bryn Parry</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">Scott Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Lisse%2C+C">Carey Lisse</a>, <a href="/search/astro-ph?searchtype=author&query=Dennerl%2C+K">Konrad Dennerl</a>, <a href="/search/astro-ph?searchtype=author&query=Jackman%2C+C+M">Caitriona M. Jackman</a>, <a href="/search/astro-ph?searchtype=author&query=Weigt%2C+D+M">Dale M. Weigt</a>, <a href="/search/astro-ph?searchtype=author&query=Porter%2C+F+S">F. Scott Porter</a>, <a href="/search/astro-ph?searchtype=author&query=Branduardi-Raymont%2C+G">Graziella Branduardi-Raymont</a>, <a href="/search/astro-ph?searchtype=author&query=Bodewits%2C+D">Dennis Bodewits</a>, <a href="/search/astro-ph?searchtype=author&query=Leppard%2C+F">Fenn Leppard</a>, <a href="/search/astro-ph?searchtype=author&query=Foster%2C+A">Adam Foster</a>, <a href="/search/astro-ph?searchtype=author&query=Gladstone%2C+G+R">G. Randall Gladstone</a>, <a href="/search/astro-ph?searchtype=author&query=Parmar%2C+V">Vatsal Parmar</a>, <a href="/search/astro-ph?searchtype=author&query=Brophy-Lee%2C+S">Stephenie Brophy-Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+C">Charly Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Ness%2C+J">Jan-Uwe Ness</a>, <a href="/search/astro-ph?searchtype=author&query=Cumbee%2C+R">Renata Cumbee</a>, <a href="/search/astro-ph?searchtype=author&query=Markevitch%2C+M">Maxim Markevitch</a>, <a href="/search/astro-ph?searchtype=author&query=Kraft%2C+R">Ralph Kraft</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.13873v2-abstract-short" style="display: inline;"> The Line Emission Mapper's (LEM's) exquisite spectral resolution and effective area will open new research domains in Astrophysics, Planetary Science and Heliophysics. LEM will provide step-change capabilities for the fluorescence, solar wind charge exchange (SWCX) and auroral precipitation processes that dominate X-ray emissions in our Solar System. The observatory will enable novel X-ray measure… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.13873v2-abstract-full').style.display = 'inline'; document.getElementById('2310.13873v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.13873v2-abstract-full" style="display: none;"> The Line Emission Mapper's (LEM's) exquisite spectral resolution and effective area will open new research domains in Astrophysics, Planetary Science and Heliophysics. LEM will provide step-change capabilities for the fluorescence, solar wind charge exchange (SWCX) and auroral precipitation processes that dominate X-ray emissions in our Solar System. The observatory will enable novel X-ray measurements of historically inaccessible line species, thermal broadening, characteristic line ratios and Doppler shifts - a universally valuable new astrophysics diagnostic toolkit. These measurements will identify the underlying compositions, conditions and physical processes from km-scale ultra-cold comets to the MK solar wind in the heliopause at 120 AU. Here, we focus on the paradigm-shifts LEM will provide for understanding the nature of the interaction between a star and its planets, especially the fundamental processes that govern the transfer of mass and energy within our Solar System, and the distribution of elements throughout the heliosphere. In this White Paper we show how LEM will enable a treasure trove of new scientific contributions that directly address key questions from the National Academies' 2023-2032 Planetary Science and 2013-2022 Heliophysics Decadal Strategies. The topics we highlight include: 1. The richest global trace element maps of the Lunar Surface ever produced; insights that address Solar System and planetary formation, and provide invaluable context ahead of Artemis and the Lunar Gateway. 2. Global maps of our Heliosphere through Solar Wind Charge Exchange (SWCX) that trace the interstellar neutral distributions in interplanetary space and measure system-wide solar wind ion abundances and velocities; a key new understanding of our local astrosphere and a synergistic complement to NASA IMAP observations of heliospheric interactions... <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.13873v2-abstract-full').style.display = 'none'; document.getElementById('2310.13873v2-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 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">White Paper for the Line Emission Mapper Astrophysics APEX X-ray Probe</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.03803">arXiv:2310.03803</a> <span> [<a href="https://arxiv.org/pdf/2310.03803">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad2fa0">10.3847/1538-4357/ad2fa0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigating Protostellar Accretion-Driven Outflows Across the Mass Spectrum: JWST NIRSpec IFU 3-5~$渭$m Spectral Mapping of Five Young Protostars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Federman%2C+S">Samuel Federman</a>, <a href="/search/astro-ph?searchtype=author&query=Megeath%2C+S+T">S. Thomas Megeath</a>, <a href="/search/astro-ph?searchtype=author&query=Rubinstein%2C+A+E">Adam E. Rubinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Gutermuth%2C+R">Robert Gutermuth</a>, <a href="/search/astro-ph?searchtype=author&query=Narang%2C+M">Mayank Narang</a>, <a href="/search/astro-ph?searchtype=author&query=Tyagi%2C+H">Himanshu Tyagi</a>, <a href="/search/astro-ph?searchtype=author&query=Manoj%2C+P">P. Manoj</a>, <a href="/search/astro-ph?searchtype=author&query=Anglada%2C+G">Guillem Anglada</a>, <a href="/search/astro-ph?searchtype=author&query=Atnagulov%2C+P">Prabhani Atnagulov</a>, <a href="/search/astro-ph?searchtype=author&query=Beuther%2C+H">Henrik Beuther</a>, <a href="/search/astro-ph?searchtype=author&query=Bourke%2C+T+L">Tyler L. Bourke</a>, <a href="/search/astro-ph?searchtype=author&query=Brunken%2C+N">Nashanty Brunken</a>, <a href="/search/astro-ph?searchtype=author&query=Garatti%2C+A+C+o">Alessio Caratti o Garatti</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+N+J">Neal J. Evans II</a>, <a href="/search/astro-ph?searchtype=author&query=Fischer%2C+W+J">William J. Fischer</a>, <a href="/search/astro-ph?searchtype=author&query=Furlan%2C+E">Elise Furlan</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+J">Joel Green</a>, <a href="/search/astro-ph?searchtype=author&query=Habel%2C+N">Nolan Habel</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+L">Lee Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=Karnath%2C+N">Nicole Karnath</a>, <a href="/search/astro-ph?searchtype=author&query=Klaassen%2C+P">Pamela Klaassen</a>, <a href="/search/astro-ph?searchtype=author&query=Linz%2C+H">Hendrik Linz</a>, <a href="/search/astro-ph?searchtype=author&query=Looney%2C+L+W">Leslie W. Looney</a>, <a href="/search/astro-ph?searchtype=author&query=Osorio%2C+M">Mayra Osorio</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+J+M">James Muzerolle Page</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="2310.03803v2-abstract-short" style="display: inline;"> Investigating Protostellar Accretion is a Cycle 1 JWST program using the NIRSpec+MIRI integral field units to obtain 2.9--28 $渭$m spectral cubes of five young protostars with luminosities of 0.2-10,000 L$_{\odot}$ in their primary accretion phase. This paper introduces the NIRSpec 2.9--5.3 $渭$m data of the inner 840-9000 au with spatial resolutions from 28-300 au. The spectra show rising continuum… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.03803v2-abstract-full').style.display = 'inline'; document.getElementById('2310.03803v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.03803v2-abstract-full" style="display: none;"> Investigating Protostellar Accretion is a Cycle 1 JWST program using the NIRSpec+MIRI integral field units to obtain 2.9--28 $渭$m spectral cubes of five young protostars with luminosities of 0.2-10,000 L$_{\odot}$ in their primary accretion phase. This paper introduces the NIRSpec 2.9--5.3 $渭$m data of the inner 840-9000 au with spatial resolutions from 28-300 au. The spectra show rising continuum emission; deep ice absorption; emission from H$_{2}$, H~I, and [Fe~II]; and the CO fundamental series in emission and absorption. Maps of the continuum emission show scattered light cavities for all five protostars. In the cavities, collimated jets are detected in [Fe~II] for the four $< 320$~L$_{\odot}$ protostars, two of which are additionally traced in Br-$伪$. Knots of [Fe~II] emission are detected toward the most luminous protostar, and knots of [FeII] emission with dynamical times of $< 30$~yrs are found in the jets of the others. While only one jet is traced in H$_2$, knots of H$_2$ and CO are detected in the jets of four protostars. H$_2$ is seen extending through the cavities, showing that they are filled by warm molecular gas. Bright H$_2$ emission is seen along the walls of a single cavity, while in three cavities narrow shells of H$_2$ emission are found, one of which has an [Fe~II] knot at its apex. These data show cavities containing collimated jets traced in atomic/ionic gas surrounded by warm molecular gas in a wide-angle wind and/or gas accelerated by bow shocks in the jets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.03803v2-abstract-full').style.display = 'none'; document.getElementById('2310.03803v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 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">26 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 966 41 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.07981">arXiv:2308.07981</a> <span> [<a href="https://arxiv.org/pdf/2308.07981">pdf</a>, <a href="https://arxiv.org/format/2308.07981">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Stable Coronal X-Ray Emission Over Twenty Years of XZ Tau </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Silverberg%2C+S+M">Steven M. Silverberg</a>, <a href="/search/astro-ph?searchtype=author&query=Guenther%2C+H+M">Hans Moritz Guenther</a>, <a href="/search/astro-ph?searchtype=author&query=Pradhan%2C+P">Pragati Pradhan</a>, <a href="/search/astro-ph?searchtype=author&query=Principe%2C+D+A">David A. Principe</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+P+C">P. C. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</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="2308.07981v1-abstract-short" style="display: inline;"> XZ Tau AB is a frequently observed binary YSO in the Taurus Molecular Cloud; XZ Tau B has been classified as an EXOr object. We present new Chandra/HETG-ACIS-S observations of XZ Tau AB, complemented with variability monitoring of the system with XMM-Newton, to constrain the variability of this system and identify high-resolution line diagnostics to better understand the underlying mechanisms that… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.07981v1-abstract-full').style.display = 'inline'; document.getElementById('2308.07981v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.07981v1-abstract-full" style="display: none;"> XZ Tau AB is a frequently observed binary YSO in the Taurus Molecular Cloud; XZ Tau B has been classified as an EXOr object. We present new Chandra/HETG-ACIS-S observations of XZ Tau AB, complemented with variability monitoring of the system with XMM-Newton, to constrain the variability of this system and identify high-resolution line diagnostics to better understand the underlying mechanisms that produce the X-rays. We observe two flares with XMM-Newton, but find that outside of these flares the coronal X-ray spectrum of XZ Tau AB is consistent over twenty years of observations. We compare the ensemble of XZ Tau X-ray observations over time with the scatter across stars observed in point-in-time observations of the Orion Nebula Cluster and find that both overlap in terms of plasma properties, i.e., some of the scatter observed in the X-ray properties of stellar ensembles stems from intrinsic source variability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.07981v1-abstract-full').style.display = 'none'; document.getElementById('2308.07981v1-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astronomical Journal. 19 pages, 11 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/2307.14056">arXiv:2307.14056</a> <span> [<a href="https://arxiv.org/pdf/2307.14056">pdf</a>, <a href="https://arxiv.org/format/2307.14056">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/stad2277">10.1093/mnras/stad2277 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The first evidence of tidally induced activity in a brown dwarf-M dwarf pair: A Chandra study of the NLTT 41135/41136 system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ili%C4%87%2C+N">Nikoleta Ili膰</a>, <a href="/search/astro-ph?searchtype=author&query=Poppenhaeger%2C+K">Katja Poppenhaeger</a>, <a href="/search/astro-ph?searchtype=author&query=Dsouza%2C+D">Desmond Dsouza</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Ag%C3%BCeros%2C+M+A">Marcel A. Ag眉eros</a>, <a href="/search/astro-ph?searchtype=author&query=Stelzer%2C+B">Beate Stelzer</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="2307.14056v1-abstract-short" style="display: inline;"> The magnetic activity of low-mass stars changes as they age. The primary process decreasing the stellar activity level is the angular momentum loss via magnetized stellar wind. However, processes like tidal interactions between stars and their close companions may slow down the braking effect and the subsequent decrease of the activity level. Until now, the tidal impact of substellar objects like… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14056v1-abstract-full').style.display = 'inline'; document.getElementById('2307.14056v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.14056v1-abstract-full" style="display: none;"> The magnetic activity of low-mass stars changes as they age. The primary process decreasing the stellar activity level is the angular momentum loss via magnetized stellar wind. However, processes like tidal interactions between stars and their close companions may slow down the braking effect and the subsequent decrease of the activity level. Until now, the tidal impact of substellar objects like brown dwarfs on the evolution of their central stars has not been quantified. Here, we analyse the X-ray properties of NLTT 41135, an M dwarf tightly orbited by a brown dwarf, to determine the impact of tidal interactions between them. We find that NLTT 41135 is more than an order of magnitude brighter in the X-ray regime than its stellar companion NLTT 41136, also an M dwarf star, with whom it forms a wide binary system. To characterize the typical intrinsic activity scatter between coeval M dwarf stars, we analyse a control sample of 25 M dwarf wide binary systems, observed with XMM-Newton and Chandra telescopes and the eROSITA instrument onboard the Spectrum R枚ntgen Gamma satellite. The activity difference in the NLTT 41135/41136 system is a $3.44 蟽$ outlier compared to the intrinsic activity scatter of the control systems. Therefore, the most convincing explanation for the observed activity discrepancy is tidal interactions between the M dwarf and its brown dwarf. This shows that tidal interactions between a star and a substellar companion can moderately alter the expected angular-momentum evolution of the star, making standard observational proxies for its age, such as X-ray emission, unreliable. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14056v1-abstract-full').style.display = 'none'; document.getElementById('2307.14056v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in MNRAS, 15 pages, 5 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/2306.11784">arXiv:2306.11784</a> <span> [<a href="https://arxiv.org/pdf/2306.11784">pdf</a>, <a href="https://arxiv.org/format/2306.11784">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"> NANCY: Next-generation All-sky Near-infrared Community surveY </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+J+J">Jiwon Jesse Han</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Price-Whelan%2C+A+M">Adrian M. Price-Whelan</a>, <a href="/search/astro-ph?searchtype=author&query=Najita%2C+J">Joan Najita</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=Saydjari%2C+A">Andrew Saydjari</a>, <a href="/search/astro-ph?searchtype=author&query=Wechsler%2C+R+H">Risa H. Wechsler</a>, <a href="/search/astro-ph?searchtype=author&query=Bonaca%2C+A">Ana Bonaca</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=Conroy%2C+C">Charlie Conroy</a>, <a href="/search/astro-ph?searchtype=author&query=Raichoor%2C+A">Anand Raichoor</a>, <a href="/search/astro-ph?searchtype=author&query=Drlica-Wagner%2C+A">Alex Drlica-Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Kollmeier%2C+J+A">Juna A. Kollmeier</a>, <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S+E">Sergey E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">Gurtina Besla</a>, <a href="/search/astro-ph?searchtype=author&query=Rix%2C+H">Hans-Walter Rix</a>, <a href="/search/astro-ph?searchtype=author&query=Goodman%2C+A">Alyssa Goodman</a>, <a href="/search/astro-ph?searchtype=author&query=Finkbeiner%2C+D">Douglas Finkbeiner</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">Abhijeet Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Ashby%2C+M">Matthew Ashby</a>, <a href="/search/astro-ph?searchtype=author&query=Bahr-Kalus%2C+B">Benedict Bahr-Kalus</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachel Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Behera%2C+J">Jayashree Behera</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=Bellm%2C+E+C">Eric C Bellm</a> , et al. (184 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="2306.11784v1-abstract-short" style="display: inline;"> The Nancy Grace Roman Space Telescope is capable of delivering an unprecedented all-sky, high-spatial resolution, multi-epoch infrared map to the astronomical community. This opportunity arises in the midst of numerous ground- and space-based surveys that will provide extensive spectroscopy and imaging together covering the entire sky (such as Rubin/LSST, Euclid, UNIONS, SPHEREx, DESI, SDSS-V, GAL… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.11784v1-abstract-full').style.display = 'inline'; document.getElementById('2306.11784v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.11784v1-abstract-full" style="display: none;"> The Nancy Grace Roman Space Telescope is capable of delivering an unprecedented all-sky, high-spatial resolution, multi-epoch infrared map to the astronomical community. This opportunity arises in the midst of numerous ground- and space-based surveys that will provide extensive spectroscopy and imaging together covering the entire sky (such as Rubin/LSST, Euclid, UNIONS, SPHEREx, DESI, SDSS-V, GALAH, 4MOST, WEAVE, MOONS, PFS, UVEX, NEO Surveyor, etc.). Roman can uniquely provide uniform high-spatial-resolution (~0.1 arcsec) imaging over the entire sky, vastly expanding the science reach and precision of all of these near-term and future surveys. This imaging will not only enhance other surveys, but also facilitate completely new science. By imaging the full sky over two epochs, Roman can measure the proper motions for stars across the entire Milky Way, probing 100 times fainter than Gaia out to the very edge of the Galaxy. Here, we propose NANCY: a completely public, all-sky survey that will create a high-value legacy dataset benefiting innumerable ongoing and forthcoming studies of the universe. NANCY is a pure expression of Roman's potential: it images the entire sky, at high spatial resolution, in a broad infrared bandpass that collects as many photons as possible. The majority of all ongoing astronomical surveys would benefit from incorporating observations of NANCY into their analyses, whether these surveys focus on nearby stars, the Milky Way, near-field cosmology, or the broader universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.11784v1-abstract-full').style.display = 'none'; document.getElementById('2306.11784v1-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 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">Submitted to the call for white papers for the Roman Core Community Survey (June 16th, 2023), and to the Bulletin of the AAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.00854">arXiv:2304.00854</a> <span> [<a href="https://arxiv.org/pdf/2304.00854">pdf</a>, <a href="https://arxiv.org/format/2304.00854">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202245467">10.1051/0004-6361/202245467 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The X-ray activity of F stars with hot Jupiters: KELT-24 versus WASP-18 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+S">S. Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">S. J. Wolk</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="2304.00854v1-abstract-short" style="display: inline;"> X-rays emitted by the coronae of solar-type stars are a feature present in up to late-A types during the main sequence phase. F stars, either with or without hot Jupiters, are usually X-ray emitters. The very low level of X-ray emission of the F5 star WASP-18 despite its relatively young age and spectral type is thus quite peculiar. [Abridged] We observed KELT-24 with \xmm\ for a total of 43 ks in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.00854v1-abstract-full').style.display = 'inline'; document.getElementById('2304.00854v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.00854v1-abstract-full" style="display: none;"> X-rays emitted by the coronae of solar-type stars are a feature present in up to late-A types during the main sequence phase. F stars, either with or without hot Jupiters, are usually X-ray emitters. The very low level of X-ray emission of the F5 star WASP-18 despite its relatively young age and spectral type is thus quite peculiar. [Abridged] We observed KELT-24 with \xmm\ for a total of 43 ks in order to test if the X-ray activity of this star is depressed by the interaction with its massive hot Jupiter, as is the case of WASP-18. KELT-24 is detected in combined EPIC images with a high significance level. Its average coronal spectrum is well described by a cool component at 0.36 keV and a hotter component at 0.98 keV. We detected a flare with a duration of about 2 ks, during which the coronal temperature reached 3.5 keV. The unabsorbed quiescent flux in 0.3-8.0 keV is $\sim1.33\times10^{-13}$ erg s$^{-1}$ cm$^{-2}$, corresponding to a luminosity of $1.5\times10^{29}$ erg s$^{-1}$ at the distance of the star. The luminosity is well within the range of the typical X-ray luminosity of F stars in Hyades, which are coeval. We conclude that the activity of KELT-24 appears normal, as expected, and is not affected by any star--planet interaction. From the analysis of TESS light curves, we infer a distribution of optical flares for KELT-24 and WASP-18. Small optical flickering similar to flares is recognized in WASP-18 but at lower levels of energy and amplitude than in KELT-24. We discuss the causes of the low activity of WASP-18. Either WASP-18b could hamper the formation of a corona bright in X-rays in its host star through some form of tidal interaction, or the star has entered a minimum of activity similar to the solar Maunder minimum. This latter hypothesis would make WASP-18 among the few candidates showing such a quench of stellar activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.00854v1-abstract-full').style.display = 'none'; document.getElementById('2304.00854v1-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, 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">6 pages, 7 figures, A&A accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.02161">arXiv:2303.02161</a> <span> [<a href="https://arxiv.org/pdf/2303.02161">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> <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="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Exploring Fundamental Particle Acceleration and Loss Processes in Heliophysics through an Orbiting X-ray Instrument in the Jovian System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+W">W. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Berland%2C+G">G. Berland</a>, <a href="/search/astro-ph?searchtype=author&query=Roussos%2C+E">E. Roussos</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+G">G. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Kollmann%2C+P">P. Kollmann</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+D">D. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+C">C. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Stallard%2C+T">T. Stallard</a>, <a href="/search/astro-ph?searchtype=author&query=Branduardi-Raymont%2C+G">G. Branduardi-Raymont</a>, <a href="/search/astro-ph?searchtype=author&query=Woodfield%2C+E+E">E. E. Woodfield</a>, <a href="/search/astro-ph?searchtype=author&query=Rae%2C+I+J">I. J. Rae</a>, <a href="/search/astro-ph?searchtype=author&query=Ray%2C+L+C">L. C. Ray</a>, <a href="/search/astro-ph?searchtype=author&query=Carter%2C+J+A">J. A. Carter</a>, <a href="/search/astro-ph?searchtype=author&query=Lindsay%2C+S+T">S. T. Lindsay</a>, <a href="/search/astro-ph?searchtype=author&query=Yao%2C+Z">Z. Yao</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+R">R. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=A.%2C+A+N+J">A. N. Jaynes A.</a>, <a href="/search/astro-ph?searchtype=author&query=Ezoe%2C+Y">Y. Ezoe</a>, <a href="/search/astro-ph?searchtype=author&query=Numazawa%2C+M">M. Numazawa</a>, <a href="/search/astro-ph?searchtype=author&query=Hospodarsky%2C+G+B">G. B. Hospodarsky</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+X">X. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Weigt%2C+D+M">D. M. Weigt</a>, <a href="/search/astro-ph?searchtype=author&query=Jackman%2C+C+M">C. M. Jackman</a>, <a href="/search/astro-ph?searchtype=author&query=Mori%2C+K">K. Mori</a>, <a href="/search/astro-ph?searchtype=author&query=N%C3%A9non%2C+Q">Q. N茅non</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="2303.02161v1-abstract-short" style="display: inline;"> Jupiter's magnetosphere is considered to be the most powerful particle accelerator in the Solar System, accelerating electrons from eV to 70 MeV and ions to GeV energies. How electromagnetic processes drive energy and particle flows, producing and removing energetic particles, is at the heart of Heliophysics. Particularly, the 2013 Decadal Strategy for Solar and Space Physics was to "Discover and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.02161v1-abstract-full').style.display = 'inline'; document.getElementById('2303.02161v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.02161v1-abstract-full" style="display: none;"> Jupiter's magnetosphere is considered to be the most powerful particle accelerator in the Solar System, accelerating electrons from eV to 70 MeV and ions to GeV energies. How electromagnetic processes drive energy and particle flows, producing and removing energetic particles, is at the heart of Heliophysics. Particularly, the 2013 Decadal Strategy for Solar and Space Physics was to "Discover and characterize fundamental processes that occur both within the heliosphere and throughout the universe". The Jovian system offers an ideal natural laboratory to investigate all of the universal processes highlighted in the previous Decadal. The X-ray waveband has been widely used to remotely study plasma across astrophysical systems. The majority of astrophysical emissions can be grouped into 5 X-ray processes: fluorescence, thermal/coronal, scattering, charge exchange and particle acceleration. The Jovian system offers perhaps the only system that presents a rich catalog of all of these X-ray emission processes and can also be visited in-situ, affording the special possibility to directly link fundamental plasma processes with their resulting X-ray signatures. This offers invaluable ground-truths for astrophysical objects beyond the reach of in-situ exploration (e.g. brown dwarfs, magnetars or galaxy clusters that map the cosmos). Here, we show how coupling in-situ measurements with in-orbit X-ray observations of Jupiter's radiation belts, Galilean satellites, Io Torus, and atmosphere addresses fundamental heliophysics questions with wide-reaching impact across helio- and astrophysics. New developments like miniaturized X-ray optics and radiation-tolerant detectors, provide compact, lightweight, wide-field X-ray instruments perfectly suited to the Jupiter system, enabling this exciting new possibility. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.02161v1-abstract-full').style.display = 'none'; document.getElementById('2303.02161v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">A White Paper for the 2024-2033 Solar and Space Physics (Heliophysics) Decadal Survey</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.07186">arXiv:2301.07186</a> <span> [<a href="https://arxiv.org/pdf/2301.07186">pdf</a>, <a href="https://arxiv.org/format/2301.07186">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/acc106">10.3847/1538-4365/acc106 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ABYSS I: Targeting strategy for APOGEE & BOSS young star survey in SDSS-V </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kounkel%2C+M">Marina Kounkel</a>, <a href="/search/astro-ph?searchtype=author&query=Zari%2C+E">Eleonora Zari</a>, <a href="/search/astro-ph?searchtype=author&query=Covey%2C+K">Kevin Covey</a>, <a href="/search/astro-ph?searchtype=author&query=Tkachenko%2C+A">Andrew Tkachenko</a>, <a href="/search/astro-ph?searchtype=author&query=Z%C3%BA%C3%B1iga%2C+C+R">Carlos Rom谩n Z煤帽iga</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K">Keivan Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Stutz%2C+A+M">Amelia M. Stutz</a>, <a href="/search/astro-ph?searchtype=author&query=Stringfellow%2C+G">Guy Stringfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">Alexandre Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">Jes煤s Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez%2C+K+P">Karla Pe帽a Ram铆rez</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">Amelia Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J+S">Jinyoung Serena Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+L">Lyra Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Kollmeier%2C+J">Juna Kollmeier</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Valdivia%2C+R">Ricardo L贸pez-Valdivia</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Ayala%2C+B">B谩rbara Rojas-Ayala</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.07186v2-abstract-short" style="display: inline;"> The fifth iteration of the Sloan Digital Sky Survey (SDSS-V) is set to obtain optical and near-infrared spectra of $\sim$5 million stars of all ages and masses throughout the Milky Way. As a part of these efforts, APOGEE & BOSS Young Star Survey (ABYSS) will observe $\sim10^5$ stars with ages $<$30 Myr that have been selected using a set of homogeneous selection functions that make use of differen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07186v2-abstract-full').style.display = 'inline'; document.getElementById('2301.07186v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.07186v2-abstract-full" style="display: none;"> The fifth iteration of the Sloan Digital Sky Survey (SDSS-V) is set to obtain optical and near-infrared spectra of $\sim$5 million stars of all ages and masses throughout the Milky Way. As a part of these efforts, APOGEE & BOSS Young Star Survey (ABYSS) will observe $\sim10^5$ stars with ages $<$30 Myr that have been selected using a set of homogeneous selection functions that make use of different tracers of youth. The ABYSS targeting strategy we describe in this paper is aimed to provide the largest spectroscopic census of young stars to-date. It consists of 8 different types of selection criteria that take the position on the HR diagram, infrared excess, variability, as well as the position in phase space in consideration. The resulting catalog of $\sim$200,000 sources (of which a half are expected to be observed) provides representative coverage of the young Galaxy, including both nearby diffuse associations as well as more distant massive complexes, reaching towards the inner Galaxy and the Galactic center. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07186v2-abstract-full').style.display = 'none'; document.getElementById('2301.07186v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 12 pages. Accepted to ApJS. Part of SDSS DR18</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.09827">arXiv:2211.09827</a> <span> [<a href="https://arxiv.org/pdf/2211.09827">pdf</a>, <a href="https://arxiv.org/format/2211.09827">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="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Line Emission Mapper (LEM): Probing the physics of cosmic ecosystems </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kraft%2C+R">Ralph Kraft</a>, <a href="/search/astro-ph?searchtype=author&query=Markevitch%2C+M">Maxim Markevitch</a>, <a href="/search/astro-ph?searchtype=author&query=Kilbourne%2C+C">Caroline Kilbourne</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J+S">Joseph S. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Akamatsu%2C+H">Hiroki Akamatsu</a>, <a href="/search/astro-ph?searchtype=author&query=Ayromlou%2C+M">Mohammadreza Ayromlou</a>, <a href="/search/astro-ph?searchtype=author&query=Bandler%2C+S+R">Simon R. Bandler</a>, <a href="/search/astro-ph?searchtype=author&query=Barbera%2C+M">Marco Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+A">Douglas A. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+A">Anil Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Biffi%2C+V">Veronica Biffi</a>, <a href="/search/astro-ph?searchtype=author&query=Bodewits%2C+D">Dennis Bodewits</a>, <a href="/search/astro-ph?searchtype=author&query=Bogdan%2C+A">Akos Bogdan</a>, <a href="/search/astro-ph?searchtype=author&query=Bonamente%2C+M">Massimiliano Bonamente</a>, <a href="/search/astro-ph?searchtype=author&query=Borgani%2C+S">Stefano Borgani</a>, <a href="/search/astro-ph?searchtype=author&query=Branduardi-Raymont%2C+G">Graziella Branduardi-Raymont</a>, <a href="/search/astro-ph?searchtype=author&query=Bregman%2C+J+N">Joel N. Bregman</a>, <a href="/search/astro-ph?searchtype=author&query=Burchett%2C+J+N">Joseph N. Burchett</a>, <a href="/search/astro-ph?searchtype=author&query=Cann%2C+J">Jenna Cann</a>, <a href="/search/astro-ph?searchtype=author&query=Carter%2C+J">Jenny Carter</a>, <a href="/search/astro-ph?searchtype=author&query=Chakraborty%2C+P">Priyanka Chakraborty</a>, <a href="/search/astro-ph?searchtype=author&query=Churazov%2C+E">Eugene Churazov</a>, <a href="/search/astro-ph?searchtype=author&query=Crain%2C+R+A">Robert A. Crain</a>, <a href="/search/astro-ph?searchtype=author&query=Cumbee%2C+R">Renata Cumbee</a>, <a href="/search/astro-ph?searchtype=author&query=Dave%2C+R">Romeel Dave</a> , et al. (85 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="2211.09827v4-abstract-short" style="display: inline;"> The Line Emission Mapper (LEM) is an X-ray Probe for the 2030s that will answer the outstanding questions of the Universe's structure formation. It will also provide transformative new observing capabilities for every area of astrophysics, and to heliophysics and planetary physics as well. LEM's main goal is a comprehensive look at the physics of galaxy formation, including stellar and black-hole… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.09827v4-abstract-full').style.display = 'inline'; document.getElementById('2211.09827v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.09827v4-abstract-full" style="display: none;"> The Line Emission Mapper (LEM) is an X-ray Probe for the 2030s that will answer the outstanding questions of the Universe's structure formation. It will also provide transformative new observing capabilities for every area of astrophysics, and to heliophysics and planetary physics as well. LEM's main goal is a comprehensive look at the physics of galaxy formation, including stellar and black-hole feedback and flows of baryonic matter into and out of galaxies. These processes are best studied in X-rays, and emission-line mapping is the pressing need in this area. LEM will use a large microcalorimeter array/IFU, covering a 30x30' field with 10" angular resolution, to map the soft X-ray line emission from objects that constitute galactic ecosystems. These include supernova remnants, star-forming regions, superbubbles, galactic outflows (such as the Fermi/eROSITA bubbles in the Milky Way and their analogs in other galaxies), the Circumgalactic Medium in the Milky Way and other galaxies, and the Intergalactic Medium at the outskirts and beyond the confines of galaxies and clusters. LEM's 1-2 eV spectral resolution in the 0.2-2 keV band will make it possible to disentangle the faintest emission lines in those objects from the bright Milky Way foreground, providing groundbreaking measurements of the physics of these plasmas, from temperatures, densities, chemical composition to gas dynamics. While LEM's main focus is on galaxy formation, it will provide transformative capability for all classes of astrophysical objects, from the Earth's magnetosphere, planets and comets to the interstellar medium and X-ray binaries in nearby galaxies, AGN, and cooling gas in galaxy clusters. In addition to pointed observations, LEM will perform a shallow all-sky survey that will dramatically expand the discovery space. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.09827v4-abstract-full').style.display = 'none'; document.getElementById('2211.09827v4-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 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. White paper for a mission concept to be submitted for the 2023 NASA Astrophysics Probes opportunity. v2: All-sky survey figure expanded, references fixed. v3: Added energy resolution measurements for prototype detector array. v4: Author list and reference fixes</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.07415">arXiv:2208.07415</a> <span> [<a href="https://arxiv.org/pdf/2208.07415">pdf</a>, <a href="https://arxiv.org/format/2208.07415">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202244268">10.1051/0004-6361/202244268 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-ray flares of the young planet host DS Tuc A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Argiroffi%2C+C">C. Argiroffi</a>, <a href="/search/astro-ph?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/astro-ph?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/astro-ph?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/astro-ph?searchtype=author&query=Reale%2C+F">F. Reale</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+S">S. Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">S. J. Wolk</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="2208.07415v1-abstract-short" style="display: inline;"> Abridged. We observed the 40 Myr old star DS Tuc A with XMM-Newton and recorded two X-ray bright flares, with the second event occurring about 12 ks after the first one. Their duration from the rise to the end of the decay was of about 8-10 ks in soft X-rays (0.3-10 keV). The flares were also recorded in the band 200-300 nm with the UVM2 filter of the Optical Monitor. The duration of the flares in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.07415v1-abstract-full').style.display = 'inline'; document.getElementById('2208.07415v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.07415v1-abstract-full" style="display: none;"> Abridged. We observed the 40 Myr old star DS Tuc A with XMM-Newton and recorded two X-ray bright flares, with the second event occurring about 12 ks after the first one. Their duration from the rise to the end of the decay was of about 8-10 ks in soft X-rays (0.3-10 keV). The flares were also recorded in the band 200-300 nm with the UVM2 filter of the Optical Monitor. The duration of the flares in UV was about 3 ks. The observed delay between the peak in the UV band and in X-rays is a probe of the heating phase followed by the evaporation and increase of density and emission measure of the flaring loop. The coronal plasma temperature at the two flare peaks reached 54-55 MK. The diagnostics based on temperatures and time scales of the flares applied to these two events allow us to infer a loop length of 5-7 x 10^10 cm, which is about the size of the stellar radius. We also infer values of electron density at the flare peaks of 2.3-6.5 x 10^11 cm^-3 , and a minimum magnetic field strength of order of 300-500 G needed to confine the plasma. The energy released during the flares was of order of 5-8 x 10^34 erg in the band 0.3-10 keV and 0.9-2.7 x 10^33 erg in the UV band (200-300 nm). We speculate that the flares were associated with Coronal Mass Ejections (CMEs) that hit the planet about 3.3 hr after the flares and dramatically increasing the rate of evaporation of the planet. From the RGS spectra we retrieved the emission measure distribution and the abundances of coronal metals during the quiescent and the flaring states. In agreement with what inferred from time resolved spectroscopy and EPIC spectra, also from the analysis of RGS spectra during the flares we infer a high electron density. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.07415v1-abstract-full').style.display = 'none'; document.getElementById('2208.07415v1-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">10 pages, 10 figures, 5 tables, accepted to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 666, A198 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.07967">arXiv:2205.07967</a> <span> [<a href="https://arxiv.org/pdf/2205.07967">pdf</a>, <a href="https://arxiv.org/format/2205.07967">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> X-rays in Cepheids: Identifying Low-Mass Companions of Intermediate-Mass Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Evans%2C+N+R">Nancy Remage Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Engle%2C+S">Scott Engle</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">Ignazio Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Guinan%2C+E">Edward Guinan</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+H+M">H. Moritz G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">Scott Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Neilson%2C+H">Hilding Neilson</a>, <a href="/search/astro-ph?searchtype=author&query=Marengo%2C+M">Massimo Marengo</a>, <a href="/search/astro-ph?searchtype=author&query=Matthews%2C+L+D">Lynn D. Matthews</a>, <a href="/search/astro-ph?searchtype=author&query=Moschou%2C+S">Sofia Moschou</a>, <a href="/search/astro-ph?searchtype=author&query=Drake%2C+J+J">Jeremy J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Winston%2C+E+M">Elaine M. Winston</a>, <a href="/search/astro-ph?searchtype=author&query=Moe%2C+M">Maxwell Moe</a>, <a href="/search/astro-ph?searchtype=author&query=Kervella%2C+P">Pierre Kervella</a>, <a href="/search/astro-ph?searchtype=author&query=Breuval%2C+L">Louise Breuval</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="2205.07967v1-abstract-short" style="display: inline;"> X-ray observations have been made of a sample of 20 classical Cepheids, including two new observations (Polaris and {\it l} Car) reported here. The occurrence of X-ray flux around the pulsation cycle is discussed. Three Cepheids are detected ($未$ Cep, $尾$ Dor, and Polaris). X-rays have also been detected from the low--mass F, G, and K companions of 4 Cepheids (V473 Lyr, R Cru, V659 Cen, and W Sgr)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.07967v1-abstract-full').style.display = 'inline'; document.getElementById('2205.07967v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.07967v1-abstract-full" style="display: none;"> X-ray observations have been made of a sample of 20 classical Cepheids, including two new observations (Polaris and {\it l} Car) reported here. The occurrence of X-ray flux around the pulsation cycle is discussed. Three Cepheids are detected ($未$ Cep, $尾$ Dor, and Polaris). X-rays have also been detected from the low--mass F, G, and K companions of 4 Cepheids (V473 Lyr, R Cru, V659 Cen, and W Sgr), and one hot companion (S Mus). Upper limits on the X-ray flux of the remaining Cepheids provide an estimate that 28\% have low mass companions. This fraction of low--mass companions in intermediate mass Cepheids is significantly lower than expected from random pairing with the field IMF. Combining the companion fraction from X-rays with that from ultraviolet observations results in a binary/multiple fraction of 57\% $\pm$12\% for Cepheids with the ratios q $>$ 0.1 and separations a $>$ 1 au. This is a lower limit since M stars are not included. X-ray observations detect less massive companions than other existing studies of intermediate mass stars. Our measured occurrence rate of unresolved, low-mass companions to Cepheids suggests that intermediate-period binaries derive from a combination of disk and core fragmentation and accretion. This yields a hybrid mass-ratio distribution that is skewed toward small values compared to a uniform distribution but is still top-heavy compared to random pairings drawn from the IMF. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.07967v1-abstract-full').style.display = 'none'; document.getElementById('2205.07967v1-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 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">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/2205.05815">arXiv:2205.05815</a> <span> [<a href="https://arxiv.org/pdf/2205.05815">pdf</a>, <a href="https://arxiv.org/format/2205.05815">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac6ef6">10.3847/1538-3881/ac6ef6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Coronal and chromospheric emission in A-type stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+H+M">Hans Moritz G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Melis%2C+C">Carl Melis</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">J. Robrade</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+P+C">P. C. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Yadav%2C+R+K">Rakesh K. Yadav</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="2205.05815v1-abstract-short" style="display: inline;"> Cool stars on the main sequence generate X-rays from coronal activity, powered by a convective dynamo. With increasing temperature, the convective envelope becomes smaller and X-ray emission fainter. We present Chandra/HRC-I observations of four single stars with early A spectral types. Only the coolest star of this sample, $蟿^3$ Eri ($T_\mathrm{eff}\approx8\,,000$ K), is detected with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.05815v1-abstract-full').style.display = 'inline'; document.getElementById('2205.05815v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.05815v1-abstract-full" style="display: none;"> Cool stars on the main sequence generate X-rays from coronal activity, powered by a convective dynamo. With increasing temperature, the convective envelope becomes smaller and X-ray emission fainter. We present Chandra/HRC-I observations of four single stars with early A spectral types. Only the coolest star of this sample, $蟿^3$ Eri ($T_\mathrm{eff}\approx8\,,000$ K), is detected with $\log(L_X/L_\mathrm{bol})=-7.6$ while the three hotter stars ($T_\mathrm{eff}\geq8\,,000$ K), namely $未$ Leo, $尾$ Leo, and $喂$ Cen, remain undetected with upper limits $\log(L_X/L_\mathrm{bol})<-8.4$. The drop in X-ray emission thus occurs in a narrow range of effective temperatures around $\sim 8100$ K and matches the drop of activity in the C III and O VI transition region lines. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.05815v1-abstract-full').style.display = 'none'; document.getElementById('2205.05815v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 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">11 pages, 3 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/2201.10465">arXiv:2201.10465</a> <span> [<a href="https://arxiv.org/pdf/2201.10465">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div 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/ac51e0">10.3847/1538-4357/ac51e0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> RW Aur A : SpeX Spectral Evidence for Differentiated Planetesimal Formation, Migration and Destruction in an 3 Myr Old Excited CTTS System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lisse%2C+C+M">C. M. Lisse</a>, <a href="/search/astro-ph?searchtype=author&query=Sitko%2C+M+L">M. L. Sitko</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">S. J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+H+M">H. M. G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Brittain%2C+S">S. Brittain</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+J+D">J. D. Green</a>, <a href="/search/astro-ph?searchtype=author&query=Steckloff%2C+J">J. Steckloff</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+B">B. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Espaillat%2C+C+C">C. C. Espaillat</a>, <a href="/search/astro-ph?searchtype=author&query=Koutoukali%2C+M">M. Koutoukali</a>, <a href="/search/astro-ph?searchtype=author&query=Moorman%2C+S+Y">S. Y. Moorman</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+A+P">A. P. Jackson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.10465v3-abstract-short" style="display: inline;"> We present 2007 - 2020 SpeX VISNIR spectral monitoring of the highly variable RW Aur A CTTS. We find direct evidence for a highly excited, IR bright, asymmetric, and time variable system. Comparison of the spectral and temporal trends found determines 5 different components: (1) a stable continuum from 0.7 - 1.3 um, with approx color temperature 4000K, produced by the CTTS photospheric surface; (2… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.10465v3-abstract-full').style.display = 'inline'; document.getElementById('2201.10465v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.10465v3-abstract-full" style="display: none;"> We present 2007 - 2020 SpeX VISNIR spectral monitoring of the highly variable RW Aur A CTTS. We find direct evidence for a highly excited, IR bright, asymmetric, and time variable system. Comparison of the spectral and temporal trends found determines 5 different components: (1) a stable continuum from 0.7 - 1.3 um, with approx color temperature 4000K, produced by the CTTS photospheric surface; (2) variable hydrogen emission lines emitted from hot excited hydrogen in the CTTSs protostellar atmosphere/accretion envelope; (3) hot CO gas in the CTTSs protostellar atmosphere/accretion envelope; (4) highly variable 1.8-5.0 um thermal continuum emission with color temperature ranging from 1130 to 1650K, due to a surrounding accretion disk that is spatially variable and has an inner wall at r = 0.04 AU and T = 1650K, and outer edges at approx 1200K; and (5) transient, bifurcated signatures of abundant Fe II + associated SI, SiI, and SrI in the systems jet structures. The bifuracted signatures first appeared in 2015, but these collapsed and disappeared into a small single peak protostellar atmosphere feature by late 2020. The temporal evolution of RW Aur As spectral signatures is consistent with a dynamically excited CTTS system forming differentiated Vesta-sized planetesimals in an asymmetric accretion disk and migrating them inward to be destructively accreted. By contrast, nearby, coeval binary companion RW Aur B evinces only (1) a stable WTTS photospheric continuum from 0.7 - 1.3 um + (3) cold CO gas in absorption + (4) stable 1.8-5.0 um thermal disk continuum emission with color temperature approx 1650K. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.10465v3-abstract-full').style.display = 'none'; document.getElementById('2201.10465v3-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> 6 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 Pages, 16 Figures, 2 Tables, accepted for publication in Astrophys J. 24-Jan-2022</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.06987">arXiv:2112.06987</a> <span> [<a href="https://arxiv.org/pdf/2112.06987">pdf</a>, <a href="https://arxiv.org/format/2112.06987">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> </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/ac2cc0">10.3847/1538-3881/ac2cc0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> What's Behind the Elephant's Trunk? Identifying Young Stellar Objects on the Outskirts of IC1396 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Silverberg%2C+S+M">Steven M. Silverberg</a>, <a href="/search/astro-ph?searchtype=author&query=Guenther%2C+H+M">Hans Moritz Guenther</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J+S">Jinyoung Serena Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Principe%2C+D+A">David A. Principe</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</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="2112.06987v1-abstract-short" style="display: inline;"> Empirically, the estimated lifetime of a typical protoplanetary disk is $<5-10$ Myr. However, the disk lifetimes required to produce a variety of observed exoplanetary systems may exceed this timescale. Some hypothesize that this inconsistency is due to estimating disk fractions at the cores of clusters, where radiation fields external to a star-disk system can photoevaporate the disk. To test thi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.06987v1-abstract-full').style.display = 'inline'; document.getElementById('2112.06987v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.06987v1-abstract-full" style="display: none;"> Empirically, the estimated lifetime of a typical protoplanetary disk is $<5-10$ Myr. However, the disk lifetimes required to produce a variety of observed exoplanetary systems may exceed this timescale. Some hypothesize that this inconsistency is due to estimating disk fractions at the cores of clusters, where radiation fields external to a star-disk system can photoevaporate the disk. To test this, we have observed a field on the western outskirts of the IC 1396 star-forming region with \textit{XMM-Newton} to identify new Class III YSO cluster members. Our X-ray sample is complete for YSOs down to $1.8\,M_{\odot}$. We use a subset of these X-ray sources that have near- and mid-infrared counterparts to determine the disk fraction for this field. We find that the fraction of X-ray-detected cluster members that host disks in the field we observe is $17_{-7}^{+10}\%$ (1$蟽$), comparable with the $29_{-3}^{+4}\%$ found in an adjacent field centered on the cometary globule IC 1396A. We re-evaluate YSO identifications in the IC 1396A field using \textit{Gaia} parallaxes compared to previous color-cut-only identifications, finding that incorporating independent distance measurements provides key additional constraints. Given the existence of at least one massive star producing an external radiation field in the cluster core, the lack of statistically significant difference in disk fraction in each observed field suggests that disk lifetimes remain consistent as a function of distance from the cluster core. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.06987v1-abstract-full').style.display = 'none'; document.getElementById('2112.06987v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, six figures. Published in Astronomical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomical Journal 162 (2021), 279 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.13382">arXiv:2105.13382</a> <span> [<a href="https://arxiv.org/pdf/2105.13382">pdf</a>, <a href="https://arxiv.org/format/2105.13382">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac05cd">10.3847/1538-3881/ac05cd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-rays in Cepheids: XMM-Newton Observations of $畏$ Aql </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Evans%2C+N+R">Nancy Remage Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">Ignazio Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Kervella%2C+P">Pierre Kervella</a>, <a href="/search/astro-ph?searchtype=author&query=Engle%2C+S">Scott Engle</a>, <a href="/search/astro-ph?searchtype=author&query=Guinan%2C+E">Edward Guinan</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+H+M">H. Moritz G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">Scott Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Neilson%2C+H">Hilding Neilson</a>, <a href="/search/astro-ph?searchtype=author&query=Marengo%2C+M">Massimo Marengo</a>, <a href="/search/astro-ph?searchtype=author&query=Matthews%2C+L+D">Lynn D. Matthews</a>, <a href="/search/astro-ph?searchtype=author&query=Moschou%2C+S">Sofia Moschou</a>, <a href="/search/astro-ph?searchtype=author&query=Drake%2C+J+J">Jeremy J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Guzik%2C+J+A">Joyce A. Guzik</a>, <a href="/search/astro-ph?searchtype=author&query=Gallenne%2C+A">Alexandre Gallenne</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9rand%2C+A">Antoine M茅rand</a>, <a href="/search/astro-ph?searchtype=author&query=Hocd%C3%A9%2C+V">Vincent Hocd茅</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.13382v1-abstract-short" style="display: inline;"> X-ray bursts have recently been discovered in the Cepheids $未$ Cep and $尾$ Dor modulated by the pulsation cycle. We have obtained an observation of the Cepheid $畏$ Aql with the XMM-Newton satellite at the phase of maximum radius, the phase at which there is a burst of X-rays in $未$ Cep. No X-rays were seen from the Cepheid $畏$ Aql at this phase, and the implications for Cepheid upper atmospheres a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13382v1-abstract-full').style.display = 'inline'; document.getElementById('2105.13382v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.13382v1-abstract-full" style="display: none;"> X-ray bursts have recently been discovered in the Cepheids $未$ Cep and $尾$ Dor modulated by the pulsation cycle. We have obtained an observation of the Cepheid $畏$ Aql with the XMM-Newton satellite at the phase of maximum radius, the phase at which there is a burst of X-rays in $未$ Cep. No X-rays were seen from the Cepheid $畏$ Aql at this phase, and the implications for Cepheid upper atmospheres are discussed. We have also used the combination of X-ray sources and Gaia and 2MASS data to search for a possible grouping around the young intermediate mass Cepheid. No indication of such a group was found. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13382v1-abstract-full').style.display = 'none'; document.getElementById('2105.13382v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/2105.08795">arXiv:2105.08795</a> <span> [<a href="https://arxiv.org/pdf/2105.08795">pdf</a>, <a href="https://arxiv.org/format/2105.08795">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="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/10.5281/zenodo.4762219">10.5281/zenodo.4762219 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> How to organize an online conference -- Lessons learned from Cool Stars 20.5 (virtually cool) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+H+M">Hans Moritz G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Davenport%2C+J+R+A">James R. A. Davenport</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">Scott Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Gallagher%2C+S">Shaun Gallagher</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.08795v1-abstract-short" style="display: inline;"> The virtual meeting was a success. Several people told us that this was "the best virtual meeting they had seen so far", which, a year into the pandemic and without a commercial provider in the back, is a great success. The biggest point of criticism was the timing: We had programming from UTC 17:00-22:00 (evening and night in central Europe, afternoon on the US East Coast, during the day in South… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.08795v1-abstract-full').style.display = 'inline'; document.getElementById('2105.08795v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.08795v1-abstract-full" style="display: none;"> The virtual meeting was a success. Several people told us that this was "the best virtual meeting they had seen so far", which, a year into the pandemic and without a commercial provider in the back, is a great success. The biggest point of criticism was the timing: We had programming from UTC 17:00-22:00 (evening and night in central Europe, afternoon on the US East Coast, during the day in South America and on the US West coast, but in the middle of the night for Asia and Australia). There is no good solution, but at least some variation in session time might go a long way to make it easier for all to attend at least some sessions. Feedback also indicates that the schedule was too compressed. Poster sessions and social contacts with the tool Gathertown worked out really well for all that used it. Our way of combining several services (Zoom for plenary and break-out rooms, Zenodo for uploading and viewing posters and proceedings, Google forms for registration and abstract submission, gathertown) allowed for a very low-cost meeting with little overhead (total cost: 600 $ for gathertown, zoom was provided through an institutional subscription, just 4 people on the LOC). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.08795v1-abstract-full').style.display = 'none'; document.getElementById('2105.08795v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.00023">arXiv:2104.00023</a> <span> [<a href="https://arxiv.org/pdf/2104.00023">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"> Great Observatories: The Past and Future of Panchromatic Astrophysics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">L. Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Megeath%2C+S+T">S. T. Megeath</a>, <a href="/search/astro-ph?searchtype=author&query=Corrales%2C+L">L. Corrales</a>, <a href="/search/astro-ph?searchtype=author&query=Marengo%2C+M">M. Marengo</a>, <a href="/search/astro-ph?searchtype=author&query=Kirkpatrick%2C+A">A. Kirkpatrick</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+J+D">J. D. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Meyer%2C+M">M. Meyer</a>, <a href="/search/astro-ph?searchtype=author&query=Gezari%2C+S">S. Gezari</a>, <a href="/search/astro-ph?searchtype=author&query=Kraft%2C+R+P">R. P. Kraft</a>, <a href="/search/astro-ph?searchtype=author&query=McCandliss%2C+S">S. McCandliss</a>, <a href="/search/astro-ph?searchtype=author&query=Tuttle%2C+S">S. Tuttle</a>, <a href="/search/astro-ph?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/astro-ph?searchtype=author&query=Bentz%2C+M">M. Bentz</a>, <a href="/search/astro-ph?searchtype=author&query=Binder%2C+B">B. Binder</a>, <a href="/search/astro-ph?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/astro-ph?searchtype=author&query=Dragomir%2C+D">D. Dragomir</a>, <a href="/search/astro-ph?searchtype=author&query=Espaillat%2C+C">C. Espaillat</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S">S. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Fox%2C+D+B">D. B. Fox</a>, <a href="/search/astro-ph?searchtype=author&query=Greenhouse%2C+M">M. Greenhouse</a>, <a href="/search/astro-ph?searchtype=author&query=Hamden%2C+E">E. Hamden</a>, <a href="/search/astro-ph?searchtype=author&query=Kauffmann%2C+J">J. Kauffmann</a>, <a href="/search/astro-ph?searchtype=author&query=Khullar%2C+G">G. Khullar</a>, <a href="/search/astro-ph?searchtype=author&query=Lazio%2C+J">J. Lazio</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a> , et al. (8 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="2104.00023v1-abstract-short" style="display: inline;"> NASA's Great Observatories have opened up the electromagnetic spectrum from space, providing sustained access to wavelengths not accessible from the ground. Together, Hubble, Compton, Chandra, and Spitzer have provided the scientific community with an agile and powerful suite of telescopes with which to attack broad scientific questions, and react to a rapidly changing scientific landscape. As the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.00023v1-abstract-full').style.display = 'inline'; document.getElementById('2104.00023v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.00023v1-abstract-full" style="display: none;"> NASA's Great Observatories have opened up the electromagnetic spectrum from space, providing sustained access to wavelengths not accessible from the ground. Together, Hubble, Compton, Chandra, and Spitzer have provided the scientific community with an agile and powerful suite of telescopes with which to attack broad scientific questions, and react to a rapidly changing scientific landscape. As the existing Great Observatories age, or are decommissioned, community access to these wavelengths will diminish, with an accompanying loss of scientific capability. This report, commissioned by the NASA Cosmic Origins, Physics of the Cosmos and Exoplanet Exploration Program Analysis Groups (PAGs), analyzes the importance of multi-wavelength observations from space during the epoch of the Great Observatories, providing examples that span a broad range of astrophysical investigations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.00023v1-abstract-full').style.display = 'none'; document.getElementById('2104.00023v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A report by the Great Observatories Science Analysis Group (SAG-10), commissioned by NASA's Cosmic Origins, Physics of the Cosmos, and Exoplanet Exploration Program Analysis Groups. 87 pages, 23 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/2103.12922">arXiv:2103.12922</a> <span> [<a href="https://arxiv.org/pdf/2103.12922">pdf</a>, <a href="https://arxiv.org/format/2103.12922">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> </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/10.1051/0004-6361/202140416">10.1051/0004-6361/202140416 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on the mass and atmospheric composition and evolution of the low-density young planet DS Tuc A b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Benatti%2C+S">S. Benatti</a>, <a href="/search/astro-ph?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/astro-ph?searchtype=author&query=Borsa%2C+F">F. Borsa</a>, <a href="/search/astro-ph?searchtype=author&query=Locci%2C+D">D. Locci</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/astro-ph?searchtype=author&query=Maggio%2C+A">A. Maggio</a>, <a href="/search/astro-ph?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">S. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/astro-ph?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/astro-ph?searchtype=author&query=Modirrousta-Galian%2C+D">D. Modirrousta-Galian</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.12922v2-abstract-short" style="display: inline;"> We performed a radial velocity (RV) monitoring of the 40 Myr old star DS Tuc A with HARPS at the ESO-3.6m to determine the planetary mass of its 8.14-days planet, first revealed by TESS. We also observed two planetary transits with HARPS and ESPRESSO at ESO-VLT, to measure the Rossiter-McLaughlin (RM) effect and characterise the planetary atmosphere. We measured the high-energy emission of the hos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12922v2-abstract-full').style.display = 'inline'; document.getElementById('2103.12922v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.12922v2-abstract-full" style="display: none;"> We performed a radial velocity (RV) monitoring of the 40 Myr old star DS Tuc A with HARPS at the ESO-3.6m to determine the planetary mass of its 8.14-days planet, first revealed by TESS. We also observed two planetary transits with HARPS and ESPRESSO at ESO-VLT, to measure the Rossiter-McLaughlin (RM) effect and characterise the planetary atmosphere. We measured the high-energy emission of the host with XMM observations to investigate models for atmospheric evaporation. We employed Gaussian Processes (GP) regression to model the high level of the stellar activity, which is more than 40 times larger than the expected RV planetary signal. We extracted the transmission spectrum of DS Tuc A b from the ESPRESSO data and searched for atmospheric elements/molecules either by single-line retrieval and by performing cross-correlation with a set of theoretical templates. Through a set of simulations, we evaluated different scenarios for the atmospheric photo-evaporation of the planet induced by the strong XUV stellar irradiation. While the stellar activity prevented us from obtaining a clear detection of the planetary signal from the RVs, we set a robust mass upper limit of 14.4 M_e for DS Tuc A b. We also confirm that the planetary system is almost (but not perfectly) aligned. The strong level of stellar activity hampers the detection of any atmospheric compounds, in line with other studies presented in the literature. The expected evolution of DS Tuc A b from our grid of models indicates that the planetary radius after the photo-evaporation phase will fall within the Fulton gap. The comparison of the available parameters of known young transiting planets with the distribution of their mature counterpart confirms that the former are characterised by a low density, with DS Tuc A b being one of the less dense. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12922v2-abstract-full').style.display = 'none'; document.getElementById('2103.12922v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 19 figures, Accepted for publication on Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 650, A66 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.07996">arXiv:2010.07996</a> <span> [<a href="https://arxiv.org/pdf/2010.07996">pdf</a>, <a href="https://arxiv.org/format/2010.07996">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abc1f1">10.3847/1538-4357/abc1f1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hubble Space Telescope Snapshot Survey for Resolved Companions of Galactic Cepheids: Final Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Evans%2C+N+R">Nancy Remage Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Guenther%2C+H+M">H. Moritz Guenther</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+H+E">Howard E. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+G+H">Gail H. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+B+D">Brian D. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Karovska%2C+M">Margarita Karovska</a>, <a href="/search/astro-ph?searchtype=author&query=Tingle%2C+E">Evan Tingle</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">Scott Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Engle%2C+S">Scott Engle</a>, <a href="/search/astro-ph?searchtype=author&query=Guinan%2C+E">Edward Guinan</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">Ignazio Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Proffitt%2C+C">Charles Proffitt</a>, <a href="/search/astro-ph?searchtype=author&query=Kervella%2C+P">Pierre Kervella</a>, <a href="/search/astro-ph?searchtype=author&query=Gallenne%2C+A">Alexandre Gallenne</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Moe%2C+M">Maxwell Moe</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.07996v1-abstract-short" style="display: inline;"> Cepheids in multiple systems provide information on the outcome of the formation of massive stars. They can also lead to exotic end-stage objects. This study concludes our survey of 70 galactic Cepheids using the {\it Hubble Space Telescope\} (\HST) Wide Field Camera~3 (WFC3) with images at two wavelengths to identify companions closer than $5\arcsec$. In the entire WFC3 survey we identify 16 prob… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.07996v1-abstract-full').style.display = 'inline'; document.getElementById('2010.07996v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.07996v1-abstract-full" style="display: none;"> Cepheids in multiple systems provide information on the outcome of the formation of massive stars. They can also lead to exotic end-stage objects. This study concludes our survey of 70 galactic Cepheids using the {\it Hubble Space Telescope\} (\HST) Wide Field Camera~3 (WFC3) with images at two wavelengths to identify companions closer than $5\arcsec$. In the entire WFC3 survey we identify 16 probable companions for 13 Cepheids. The seven Cepheids having resolved candidate companions within $2"$ all have the surprising property of themselves being spectroscopic binaries (as compared with a 29\% incidence of spectroscopic binaries in the general Cepheid population). That is a strong suggestion that an inner binary is linked to the scenario of a third companion within a few hundred~AU\null. This characteristic is continued for more widely separated companions. Under a model where the outer companion is formed first, it is unlikely that it can anticipate a subsequent inner binary. Rather it is more likely that a triple system has undergone dynamical interaction, resulting in one star moving outward to its current location. {\it Chandra\} and {\it Gaia\} data as well as radial velocities and \HSTSTIS and {\it IUE\} spectra are used to derive properties of the components of the Cepheid systems. The colors of the companion candidates show a change in distribution at approximately 2000~AU separations, from a range including both hot and cool colors for closer companions, to only low-mass companions for wider separations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.07996v1-abstract-full').style.display = 'none'; document.getElementById('2010.07996v1-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 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/2008.06425">arXiv:2008.06425</a> <span> [<a href="https://arxiv.org/pdf/2008.06425">pdf</a>, <a href="https://arxiv.org/format/2008.06425">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="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> X-ray Studies of Planetary Systems: A 2020 Decadal Survey White Paper </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hong%2C+J">Jaesub Hong</a>, <a href="/search/astro-ph?searchtype=author&query=Romaine%2C+S">Suzanne Romaine</a>, <a href="/search/astro-ph?searchtype=author&query=Nittler%2C+L">Larry Nittler</a>, <a href="/search/astro-ph?searchtype=author&query=Elvis%2C+M">Martin Elvis</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+I">Ian Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Branduardi-Raymont%2C+G">Graziella Branduardi-Raymont</a>, <a href="/search/astro-ph?searchtype=author&query=Rim%2C+L">Lucy Rim</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">Scott Wolk</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2008.06425v1-abstract-short" style="display: inline;"> Whether it is fluorescence emission from asteroids and moons, solar wind charge exchange from comets, exospheric escape from Mars, pion reactions on Venus, sprite lighting on Saturn, or the Io plasma torus in the Jovian magnetosphere, the Solar System is surprisingly rich and diverse in X-ray emitting objects. The compositions of diverse planetary bodies are of fundamental interest to planetary sc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.06425v1-abstract-full').style.display = 'inline'; document.getElementById('2008.06425v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.06425v1-abstract-full" style="display: none;"> Whether it is fluorescence emission from asteroids and moons, solar wind charge exchange from comets, exospheric escape from Mars, pion reactions on Venus, sprite lighting on Saturn, or the Io plasma torus in the Jovian magnetosphere, the Solar System is surprisingly rich and diverse in X-ray emitting objects. The compositions of diverse planetary bodies are of fundamental interest to planetary science, providing clues to the formation and evolutionary history of the target bodies and the solar system as a whole. X-ray fluorescence (XRF) lines, triggered either by solar X-rays or energetic ions, are intrinsic to atomic energy levels and carry an unambiguous signature of the elemental composition of the emitting bodies. All remote-sensing XRF spectrometers used so far on planetary orbiters have been collimated instruments, with limited achievable spatial resolution, and many have used archaic X-ray detectors with poor energy resolution. Focusing X-ray optics provide true spectroscopic imaging and are used widely in astrophysics missions, but until now their mass and volume have been too large for resource-limited in-situ planetary missions. Recent advances in X-ray instrumentation such as the Micro-Pore Optics used on the BepiColombo X-ray instrument (Fraser et al., 2010), Miniature X-ray Optics (Hong et al., 2016) and highly radiation tolerant CMOS X-ray sensors (e.g., Kenter et al., 2012) enable compact, yet powerful, truly focusing X-ray Imaging Spectrometers. Such instruments will enable compositional measurements of planetary bodies with much better spatial resolution and thus open a large new discovery space in planetary science, greatly enhancing our understanding of the nature and origin of diverse planetary bodies. Here, we discuss many examples of the power of XRF to address key science questions across the solar system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.06425v1-abstract-full').style.display = 'none'; document.getElementById('2008.06425v1-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 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">cover + 7 pages, 3 figures, submitted as a white paper to Planetary Science and Astrobiology Decadal Survey 2023-2032</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.05466">arXiv:2005.05466</a> <span> [<a href="https://arxiv.org/pdf/2005.05466">pdf</a>, <a href="https://arxiv.org/format/2005.05466">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/ab92a2">10.3847/1538-4357/ab92a2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Star-Gas Surface Density Correlations in Twelve Nearby Molecular Clouds I: Data Collection and Star-Sampled Analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pokhrel%2C+R">Riwaj Pokhrel</a>, <a href="/search/astro-ph?searchtype=author&query=Gutermuth%2C+R+A">Robert A. Gutermuth</a>, <a href="/search/astro-ph?searchtype=author&query=Betti%2C+S+K">Sarah K. Betti</a>, <a href="/search/astro-ph?searchtype=author&query=Offner%2C+S+S+R">Stella S. R. Offner</a>, <a href="/search/astro-ph?searchtype=author&query=Myers%2C+P+C">Philip C. Myers</a>, <a href="/search/astro-ph?searchtype=author&query=Megeath%2C+S+T">S. Thomas Megeath</a>, <a href="/search/astro-ph?searchtype=author&query=Sokol%2C+A+D">Alyssa D. Sokol</a>, <a href="/search/astro-ph?searchtype=author&query=Ali%2C+B">Babar Ali</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+L">Lori Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+T+S">Tom S. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Dunham%2C+M+M">Michael M. Dunham</a>, <a href="/search/astro-ph?searchtype=author&query=Fischer%2C+W+J">William J. Fischer</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">Thomas Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Heyer%2C+M">Mark Heyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hora%2C+J+L">Joseph L. Hora</a>, <a href="/search/astro-ph?searchtype=author&query=Pipher%2C+J+L">Judith L. Pipher</a>, <a href="/search/astro-ph?searchtype=author&query=Tobin%2C+J+J">John J. Tobin</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</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="2005.05466v1-abstract-short" style="display: inline;"> We explore the relation between the stellar mass surface density and the mass surface density of molecular hydrogen gas in twelve nearby molecular clouds that are located at $<$1.5 kpc distance. The sample clouds span an order of magnitude range in mass, size, and star formation rates. We use thermal dust emission from $Herschel$ maps to probe the gas surface density and the young stellar objects… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.05466v1-abstract-full').style.display = 'inline'; document.getElementById('2005.05466v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.05466v1-abstract-full" style="display: none;"> We explore the relation between the stellar mass surface density and the mass surface density of molecular hydrogen gas in twelve nearby molecular clouds that are located at $<$1.5 kpc distance. The sample clouds span an order of magnitude range in mass, size, and star formation rates. We use thermal dust emission from $Herschel$ maps to probe the gas surface density and the young stellar objects from the most recent $Spitzer$ Extended Solar Neighborhood Archive (SESNA) catalog to probe the stellar surface density. Using a star-sampled nearest neighbor technique to probe the star-gas surface density correlations at the scale of a few parsecs, we find that the stellar mass surface density varies as a power-law of the gas mass surface density, with a power-law index of $\sim$2 in all the clouds. The consistent power-law index implies that star formation efficiency is directly correlated with gas column density, and no gas column density threshold for star formation is observed. We compare the observed correlations with the predictions from an analytical model of thermal fragmentation, and with the synthetic observations of a recent hydrodynamic simulation of a turbulent star-forming molecular cloud. We find that the observed correlations are consistent for some clouds with the thermal fragmentation model and can be reproduced using the hydrodynamic simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.05466v1-abstract-full').style.display = 'none'; document.getElementById('2005.05466v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 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">39 pages, 10 figures, 3 tables. Accepted 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/2003.06870">arXiv:2003.06870</a> <span> [<a href="https://arxiv.org/pdf/2003.06870">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div 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/ab7b80">10.3847/1538-4357/ab7b80 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HD 145263: Spectral Observations of Silica Debris Disk Formation via Extreme Space Weathering? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lisse%2C+C+M">C. M. Lisse</a>, <a href="/search/astro-ph?searchtype=author&query=Meng%2C+H+Y+A">H. Y. A. Meng</a>, <a href="/search/astro-ph?searchtype=author&query=Sitko%2C+M+L">M. L. Sitko</a>, <a href="/search/astro-ph?searchtype=author&query=Morlok%2C+A">A. Morlok</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+B+C">B. C. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+A+P">A. P. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Vervack%2C+R+J">R. J. Vervack Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+C+H">C. H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">S. J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+M+D">M. D. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Marengo%2C+M">M. Marengo</a>, <a href="/search/astro-ph?searchtype=author&query=Britt%2C+D+T">D. T. Britt</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2003.06870v1-abstract-short" style="display: inline;"> We report here time domain infrared spectroscopy and optical photometry of the HD145263 silica-rich circumstellar disk system taken from 2003 through 2014. We find an F4V host star surrounded by a stable, massive 1e22 - 1e23 kg (M_Moon to M_Mars) dust disk. No disk gas was detected, and the primary star was seen rotating with a rapid ~1.75 day period. After resolving a problem with previously repo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.06870v1-abstract-full').style.display = 'inline'; document.getElementById('2003.06870v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.06870v1-abstract-full" style="display: none;"> We report here time domain infrared spectroscopy and optical photometry of the HD145263 silica-rich circumstellar disk system taken from 2003 through 2014. We find an F4V host star surrounded by a stable, massive 1e22 - 1e23 kg (M_Moon to M_Mars) dust disk. No disk gas was detected, and the primary star was seen rotating with a rapid ~1.75 day period. After resolving a problem with previously reported observations, we find the silica, Mg-olivine, and Fe-pyroxene mineralogy of the dust disk to be stable throughout, and very unusual compared to the ferromagnesian silicates typically found in primordial and debris disks. By comparison with mid-infrared spectral features of primitive solar system dust, we explore the possibility that HD 145263's circumstellar dust mineralogy occurred with preferential destruction of Fe-bearing olivines, metal sulfides, and water ice in an initially comet-like mineral mix and their replacement by Fe-bearing pyroxenes, amorphous pyroxene, and silica. We reject models based on vaporizing optical stellar megaflares, aqueous alteration, or giant hypervelocity impacts as unable to produce the observed mineralogy. Scenarios involving unusually high Si abundances are at odds with the normal stellar absorption near-infrared feature strengths for Mg, Fe, and Si. Models involving intense space weathering of a thin surface patina via moderate (T < 1300 K) heating and energetic ion sputtering due to a stellar superflare from the F4V primary are consistent with the observations. The space weathered patina should be reddened, contain copious amounts of nanophase Fe, and should be transient on timescales of decades unless replenished. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.06870v1-abstract-full').style.display = 'none'; document.getElementById('2003.06870v1-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 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">41 Pages, 5 Figures, 5 Tables, Accepted for publication in 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/2002.05838">arXiv:2002.05838</a> <span> [<a href="https://arxiv.org/pdf/2002.05838">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Planetary Science with Astrophysical Assets: Defining the Core Capabilities of Platforms </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+J">James Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Milam%2C+S">Stefanie Milam</a>, <a href="/search/astro-ph?searchtype=author&query=Bjoraker%2C+G">Gordon Bjoraker</a>, <a href="/search/astro-ph?searchtype=author&query=Carey%2C+S">Sean Carey</a>, <a href="/search/astro-ph?searchtype=author&query=Daou%2C+D">Doris Daou</a>, <a href="/search/astro-ph?searchtype=author&query=Fletcher%2C+L">Leigh Fletcher</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+W">Walt Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Hartogh%2C+P">Paul Hartogh</a>, <a href="/search/astro-ph?searchtype=author&query=Hartzell%2C+C">Christine Hartzell</a>, <a href="/search/astro-ph?searchtype=author&query=Hendrix%2C+A">Amanda Hendrix</a>, <a href="/search/astro-ph?searchtype=author&query=Nugent%2C+C">Carrie Nugent</a>, <a href="/search/astro-ph?searchtype=author&query=Rivkin%2C+A">Andy Rivkin</a>, <a href="/search/astro-ph?searchtype=author&query=Swindle%2C+T">Timothy Swindle</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+C">Cristina Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Tiscareno%2C+M">Matthew Tiscareno</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+G">Geronimo Villanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">Scott Wolk</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="2002.05838v1-abstract-short" style="display: inline;"> We seek to compile a uniform set of basic capabilities and needs to maximize the yield of Solar System science with future Astrophysics assets while allowing those assets to achieve their Astrophysics priorities. Within considerations of cost and complexity, inclusion of capabilities that make a particular platform useable to planetary science provide a critical advantage over platforms lacking su… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.05838v1-abstract-full').style.display = 'inline'; document.getElementById('2002.05838v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.05838v1-abstract-full" style="display: none;"> We seek to compile a uniform set of basic capabilities and needs to maximize the yield of Solar System science with future Astrophysics assets while allowing those assets to achieve their Astrophysics priorities. Within considerations of cost and complexity, inclusion of capabilities that make a particular platform useable to planetary science provide a critical advantage over platforms lacking such capabilities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.05838v1-abstract-full').style.display = 'none'; document.getElementById('2002.05838v1-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 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">Small Bodies Assessment Group Committee on Planetary Science with Astrophysical Assets, submitted to The National Academies of Science, Engineering, and Medicine艣 Call to the Astronomy and Astrophysics Community for Science White 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/2001.02253">arXiv:2001.02253</a> <span> [<a href="https://arxiv.org/pdf/2001.02253">pdf</a>, <a href="https://arxiv.org/format/2001.02253">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ab7121">10.3847/1538-3881/ab7121 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-ray Observations of the Peculiar Cepheid V473 Lyr Identify A Low-Mass Companion </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Evans%2C+N+R">Nancy Remage Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">Ignazio Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Molnar%2C+L">Laszlo Molnar</a>, <a href="/search/astro-ph?searchtype=author&query=Szabados%2C+L">Laszlo Szabados</a>, <a href="/search/astro-ph?searchtype=author&query=Plachy%2C+E">Emese Plachy</a>, <a href="/search/astro-ph?searchtype=author&query=Szabo%2C+R">Robert Szabo</a>, <a href="/search/astro-ph?searchtype=author&query=Engle%2C+S">Scott Engle</a>, <a href="/search/astro-ph?searchtype=author&query=Guinan%2C+E">Ed Guinan</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">Scott Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Guenther%2C+H+M">H. Moritz Guenther</a>, <a href="/search/astro-ph?searchtype=author&query=Neilson%2C+H">Hilding Neilson</a>, <a href="/search/astro-ph?searchtype=author&query=Marengo%2C+M">Massimo Marengo</a>, <a href="/search/astro-ph?searchtype=author&query=Matthews%2C+L+D">Lynn D. Matthews</a>, <a href="/search/astro-ph?searchtype=author&query=Moschou%2C+S">Sofia Moschou</a>, <a href="/search/astro-ph?searchtype=author&query=Drake%2C+J+J">Jeremy J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Kashyap%2C+V">Vinay Kashyap</a>, <a href="/search/astro-ph?searchtype=author&query=Kervella%2C+P">Pierre Kervella</a>, <a href="/search/astro-ph?searchtype=author&query=Tordai%2C+T">Tamas Tordai</a>, <a href="/search/astro-ph?searchtype=author&query=Somogyi%2C+P">Peter Somogyi</a>, <a href="/search/astro-ph?searchtype=author&query=Burki%2C+G">Gilbert Burki</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.02253v1-abstract-short" style="display: inline;"> V473 Lyr is a classical Cepheid which is unique in having substantial amplitude variations with a period of approximately 3.3 years, thought to be similar to the Blazhko variations in RR Lyrae stars. We obtained an {\it XMM-Newton} observation of this star to followup a previous detection in X-rays. Rather than the X-ray burst and rapid decline near maximum radius seen in $未$ Cephei itself, the X-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.02253v1-abstract-full').style.display = 'inline'; document.getElementById('2001.02253v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.02253v1-abstract-full" style="display: none;"> V473 Lyr is a classical Cepheid which is unique in having substantial amplitude variations with a period of approximately 3.3 years, thought to be similar to the Blazhko variations in RR Lyrae stars. We obtained an {\it XMM-Newton} observation of this star to followup a previous detection in X-rays. Rather than the X-ray burst and rapid decline near maximum radius seen in $未$ Cephei itself, the X-ray flux in V473 Lyr remained constant for a third of the pulsation cycle covered by the observation. Thus the X-rays are most probably not produced by the changes around the pulsation cycle. The X-ray spectrum is soft (kT = 0.6 keV), with X-ray properties which are consistent with a young low mass companion. Previously there was no evidence of a companion in radial velocities or in {\it Gaia} and {\it Hipparcos} proper motions. While this rules out companions which are very close or very distant, a binary companion at a separation between 30 and 300 AU is possible. This is an example of an X-ray observation revealing evidence of a low mass companion, which is important in completing the mass ratio statistics of binary Cepheids. Furthermore, the detection of a young X-ray bright companion is a further indication that the Cepheid (primary) is a Population I star, even though its pulsation behavior differs from other classical Cepheids. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.02253v1-abstract-full').style.display = 'none'; document.getElementById('2001.02253v1-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/1909.13747">arXiv:1909.13747</a> <span> [<a href="https://arxiv.org/pdf/1909.13747">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"> Astro2020 APC White Paper: SmallSats for Astrophysics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">David R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Freeman%2C+A">Anthony Freeman</a>, <a href="/search/astro-ph?searchtype=author&query=Gaier%2C+T">Todd Gaier</a>, <a href="/search/astro-ph?searchtype=author&query=Gorjian%2C+V">Varoujan Gorjian</a>, <a href="/search/astro-ph?searchtype=author&query=Shkolnik%2C+E">Evgenya Shkolnik</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">Scott Wolk</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="1909.13747v1-abstract-short" style="display: inline;"> The commercial SmallSat industry is booming and has developed numerous low-cost, capable satellite buses. SmallSats can be used as vehicles for technology development or to host science missions. Missions hosted on SmallSats can answer specific science questions that are difficult or impossible to answer with larger facilities, can be developed relatively quickly, serve to train engineering and sc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.13747v1-abstract-full').style.display = 'inline'; document.getElementById('1909.13747v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.13747v1-abstract-full" style="display: none;"> The commercial SmallSat industry is booming and has developed numerous low-cost, capable satellite buses. SmallSats can be used as vehicles for technology development or to host science missions. Missions hosted on SmallSats can answer specific science questions that are difficult or impossible to answer with larger facilities, can be developed relatively quickly, serve to train engineering and scientists, and provide access to space for small institutions. SmallSats complement larger Astrophysics missions and allow the broader community to test new ideas at the bottom of the market, creating new capabilities which find their way to larger missions. Currently, NASA Astrophysics does not provide flight opportunities that would allow technology maturation of instrument systems or concepts of operations. Without flight opportunities to mature technologies, missions hosted on SmallSats are likely to be considered high risk, and face long odds being selected for implementation. Our primary suggestion is that NASA decouples science and technology for SmallSats by creating a technology-based SmallSat AO, modeled after the Earth Sciences InVEST call. Such AO would help reduce the new technology risk for science missions of any size. We also suggest that NASA provides additional science-driven SmallSat opportunities at the ~$12M funding level, provides access to new launchers free of charge to proposers, and re-structures the solicitation AOs so that SmallSats do not compete with other mission classes such as balloons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.13747v1-abstract-full').style.display = 'none'; document.getElementById('1909.13747v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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, 2 figures, APC White Paper submitted to the Astro2020 Decadal Survey (Additional endorsers listed in article)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.04320">arXiv:1904.04320</a> <span> [<a href="https://arxiv.org/pdf/1904.04320">pdf</a>, <a href="https://arxiv.org/format/1904.04320">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"> X-ray Studies of Exoplanets: A 2020 Decadal Survey White Paper </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Drake%2C+J+J">Jeremy J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Branduardi-Raymont%2C+G">Graziella Branduardi-Raymont</a>, <a href="/search/astro-ph?searchtype=author&query=Poppenhaeger%2C+K">Katja Poppenhaeger</a>, <a href="/search/astro-ph?searchtype=author&query=Airapetian%2C+V">Vladimir Airapetian</a>, <a href="/search/astro-ph?searchtype=author&query=France%2C+K">Kevin France</a>, <a href="/search/astro-ph?searchtype=author&query=Sciortino%2C+S">Salvatore Sciortino</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">Ignazio Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Osten%2C+R+A">Rachel A. Osten</a>, <a href="/search/astro-ph?searchtype=author&query=Lisse%2C+C+M">Carey M. Lisse</a>, <a href="/search/astro-ph?searchtype=author&query=Kashyap%2C+V">Vinay Kashyap</a>, <a href="/search/astro-ph?searchtype=author&query=Wargelin%2C+B">Brad Wargelin</a>, <a href="/search/astro-ph?searchtype=author&query=Wood%2C+B">Brian Wood</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+W">Willaim Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Principe%2C+D">David Principe</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+M">Moritz G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Christian%2C+D+J">Damian J. Christian</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarado-Gomez%2C+J+D">Julian David Alvarado-Gomez</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+C">Chuanfei Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L">Lidia Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Karovska%2C+M">Margarita Karovska</a>, <a href="/search/astro-ph?searchtype=author&query=Moschou%2C+S+P">Sofia P. Moschou</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+P+K">Peter K. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R">Randall Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Snios%2C+B">Bradford Snios</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="1904.04320v1-abstract-short" style="display: inline;"> Over the last two decades, the discovery of exoplanets has fundamentally changed our perception of the universe and humanity's place within it. Recent work indicates that a solar system's X-ray and high energy particle environment is of fundamental importance to the formation and development of the atmospheres of close-in planets such as hot Jupiters, and Earth-like planets around M stars. X-ray i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.04320v1-abstract-full').style.display = 'inline'; document.getElementById('1904.04320v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.04320v1-abstract-full" style="display: none;"> Over the last two decades, the discovery of exoplanets has fundamentally changed our perception of the universe and humanity's place within it. Recent work indicates that a solar system's X-ray and high energy particle environment is of fundamental importance to the formation and development of the atmospheres of close-in planets such as hot Jupiters, and Earth-like planets around M stars. X-ray imaging and spectroscopy provide powerful and unique windows into the high energy flux that an exoplanet experiences, and X-ray photons also serve as proxies for potentially transfigurative coronal mass ejections. Finally, if the host star is a bright enough X-ray source, transit measurements akin to those in the optical and infrared are possible and allow for direct characterization of the upper atmospheres of exoplanets. In this brief white paper, we discuss contributions to the study of exoplanets and their environs which can be made by X-ray data of increasingly high quality that are achievable in the next 10--15 years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.04320v1-abstract-full').style.display = 'none'; document.getElementById('1904.04320v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">7 pages with 2 figures. A 2020 Decadal Survey 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/1904.04319">arXiv:1904.04319</a> <span> [<a href="https://arxiv.org/pdf/1904.04319">pdf</a>, <a href="https://arxiv.org/format/1904.04319">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> <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"> Understanding Galactic Star Formation with Next Generation X-ray Spectroscopy and Imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Osten%2C+R">Rachel Osten</a>, <a href="/search/astro-ph?searchtype=author&query=Brickhouse%2C+N">Nancy Brickhouse</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+M">Moritz G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Drake%2C+J">Jeremy Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Winston%2C+E">Elaine Winston</a>, <a href="/search/astro-ph?searchtype=author&query=Leahy%2C+D">Denis Leahy</a>, <a href="/search/astro-ph?searchtype=author&query=Tzanavaris%2C+P">Panayiotis Tzanavaris</a>, <a href="/search/astro-ph?searchtype=author&query=Principe%2C+D+A">David A. Principe</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="1904.04319v1-abstract-short" style="display: inline;"> This white paper is motivated by open questions in star formation, which can be uniquely addressed by high resolution X-ray imaging and require an X-ray observatory with large collecting area along good spectral resolution. A complete census of star-forming regions in X-rays, combined with well matched infrared (IR) data, will advance our understanding of disk survival times and dissipation mechan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.04319v1-abstract-full').style.display = 'inline'; document.getElementById('1904.04319v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.04319v1-abstract-full" style="display: none;"> This white paper is motivated by open questions in star formation, which can be uniquely addressed by high resolution X-ray imaging and require an X-ray observatory with large collecting area along good spectral resolution. A complete census of star-forming regions in X-rays, combined with well matched infrared (IR) data, will advance our understanding of disk survival times and dissipation mechanisms. In addition, we will be able to directly observe the effects of X-ray irradiation on circumstellar grain growth to compare with grain evolution models in both high- and low-UV environments. X-rays are native to stars at all phases of star formation and affect planet-forming disks especially through flares. Moreover, X-rays trace magnetic fields which weave through the flares, providing a unique, non-gravitational feedback mechanism between disk and star. Finally, the bright X-ray emission emanating from hot plasma associated with massive stars can have large scale impacts on the topology of star-forming regions and their interface with the interstellar medium (ISM). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.04319v1-abstract-full').style.display = 'none'; document.getElementById('1904.04319v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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 Science White Paper, 3 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/1903.12338">arXiv:1903.12338</a> <span> [<a href="https://arxiv.org/pdf/1903.12338">pdf</a>, <a href="https://arxiv.org/format/1903.12338">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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"> High-Energy Photon and Particle Effects onExoplanet Atmospheres and Habitability </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Drake%2C+J+J">Jeremy J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarado-G%C3%B3mez%2C+J+D">Juli谩n D. Alvarado-G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Airapetian%2C+V">Vladimir Airapetian</a>, <a href="/search/astro-ph?searchtype=author&query=Cauley%2C+P+W">P. Wilson Cauley</a>, <a href="/search/astro-ph?searchtype=author&query=Argiroffi%2C+C">Costanza Argiroffi</a>, <a href="/search/astro-ph?searchtype=author&query=Browning%2C+M+K">Matthew K. Browning</a>, <a href="/search/astro-ph?searchtype=author&query=Christian%2C+D+J">Damian J. Christian</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+O">Ofer Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Corrales%2C+L">Lia Corrales</a>, <a href="/search/astro-ph?searchtype=author&query=Danchi%2C+W">William Danchi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Val-Borro%2C+M">Miguel de Val-Borro</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+C">Chuanfei Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Forman%2C+W">William Forman</a>, <a href="/search/astro-ph?searchtype=author&query=France%2C+K">Kevin France</a>, <a href="/search/astro-ph?searchtype=author&query=Gallo%2C+E">Elena Gallo</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Sage%2C+K">Katherine Garcia-Sage</a>, <a href="/search/astro-ph?searchtype=author&query=Garraffo%2C+C">Cecilia Garraffo</a>, <a href="/search/astro-ph?searchtype=author&query=Gelino%2C+D+M">Dawn M. Gelino</a>, <a href="/search/astro-ph?searchtype=author&query=Gronoff%2C+G">Guillaume Gronoff</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+H+M">H. Moritz G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Harper%2C+G+M">Graham M. Harper</a>, <a href="/search/astro-ph?searchtype=author&query=Haywood%2C+R+D">Rapha毛lle D. Haywood</a>, <a href="/search/astro-ph?searchtype=author&query=Karovska%2C+M">Margarita Karovska</a>, <a href="/search/astro-ph?searchtype=author&query=Kashyap%2C+V">Vinay Kashyap</a>, <a href="/search/astro-ph?searchtype=author&query=Kastner%2C+J">Joel Kastner</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="1903.12338v1-abstract-short" style="display: inline;"> It is now recognized that energetic stellar photon and particle radiation evaporates and erodes planetary atmospheres and controls upper atmospheric chemistry. Key exoplanet host stars will be too faint at X-ray wavelengths for accurate characterization using existing generation and future slated X-ray telescopes. Observation of stellar coronal mass ejections and winds are also beyond current inst… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.12338v1-abstract-full').style.display = 'inline'; document.getElementById('1903.12338v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.12338v1-abstract-full" style="display: none;"> It is now recognized that energetic stellar photon and particle radiation evaporates and erodes planetary atmospheres and controls upper atmospheric chemistry. Key exoplanet host stars will be too faint at X-ray wavelengths for accurate characterization using existing generation and future slated X-ray telescopes. Observation of stellar coronal mass ejections and winds are also beyond current instrumentation. In line with theCommittee on an Exoplanet Science Strategy recognition that holistic observational approaches are needed, we point out here that a full understanding of exoplanet atmospheres, their evolution and determination of habitability requires a powerful high-resolution X-ray imaging and spectroscopic observatory. This is the only capability that can: (1) characterize by proxy the crucial, difficult to observe, EUV stellar flux, its history and its variations for planet hosting stars; (2) observe the stellar wind; (3) detect the subtle Doppler signatures of coronal mass ejections. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.12338v1-abstract-full').style.display = 'none'; document.getElementById('1903.12338v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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 Science 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/1903.09540">arXiv:1903.09540</a> <span> [<a href="https://arxiv.org/pdf/1903.09540">pdf</a>, <a href="https://arxiv.org/format/1903.09540">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The fastest components in stellar jets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+H+M">Hans Moritz G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Espaillat%2C+C">Catherine Espaillat</a>, <a href="/search/astro-ph?searchtype=author&query=France%2C+K">Kevin France</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Zhi-Yun Li</a>, <a href="/search/astro-ph?searchtype=author&query=Johns--Krull%2C+C+M">Christopher M. Johns--Krull</a>, <a href="/search/astro-ph?searchtype=author&query=Dougados%2C+C">Catherine Dougados</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+P+C">P. Christian Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Fischer%2C+W">Will Fischer</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+T+L">Tracy L. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCdel%2C+M">Manuel G眉del</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="1903.09540v1-abstract-short" style="display: inline;"> Young stars accrete mass from a circumstellar disk, but at the same time disk and star eject outflows and jets. These outflows have an onion-like structure where the innermost and fastest layers are surrounded by increasingly lower velocity components. The outer layers are probably photo-evaporative and magnetocentrifugally launched disk winds, but the nature of the inner winds is still uncertain.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.09540v1-abstract-full').style.display = 'inline'; document.getElementById('1903.09540v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.09540v1-abstract-full" style="display: none;"> Young stars accrete mass from a circumstellar disk, but at the same time disk and star eject outflows and jets. These outflows have an onion-like structure where the innermost and fastest layers are surrounded by increasingly lower velocity components. The outer layers are probably photo-evaporative and magnetocentrifugally launched disk winds, but the nature of the inner winds is still uncertain. Since the fastest components carry only a small fraction of the mass, they are best observed at high-energies (X-ray and UV) as the slower, more massive components do not reach plasma temperatures sufficient for relevant X-ray or UV emission. Outflows are the most likely way in which a star or its disk can shed angular momentum and allow accretion to proceed; thus we cannot understand the accretion and the rotation rate of young stars if we cannot solve the origin of the inner jet components. Stellar jets share characteristics with their counterparts in more massive astrophysical objects, such as stellar mass black holes and AGN, with the added benefit that young stars are found at much closer distances and thus scales not accessible in other types of objects can be resolved. To understand the origin and impact of the inner jets, sub-arcsecond imaging and spectroscopy in the UV and X-rays is required, together with theory and modelling to interpret existing and future observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.09540v1-abstract-full').style.display = 'none'; document.getElementById('1903.09540v1-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 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Submitted to the 2020 Astronomy decadal survey as science 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/1903.06634">arXiv:1903.06634</a> <span> [<a href="https://arxiv.org/pdf/1903.06634">pdf</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="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Increasing the Discovery Space in Astrophysics - A Collation of Six Submitted White Papers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fabbiano%2C+G">G. Fabbiano</a>, <a href="/search/astro-ph?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/astro-ph?searchtype=author&query=Accomazzi%2C+A">A. Accomazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Berriman%2C+G+B">G. B. Berriman</a>, <a href="/search/astro-ph?searchtype=author&query=Brickhouse%2C+N">N. Brickhouse</a>, <a href="/search/astro-ph?searchtype=author&query=Bose%2C+S">S. Bose</a>, <a href="/search/astro-ph?searchtype=author&query=Carrera%2C+D">D. Carrera</a>, <a href="/search/astro-ph?searchtype=author&query=Chilingarian%2C+I">I. Chilingarian</a>, <a href="/search/astro-ph?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/astro-ph?searchtype=author&query=Czerny%2C+B">B. Czerny</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Abrusco%2C+R">R. D'Abrusco</a>, <a href="/search/astro-ph?searchtype=author&query=Diemer%2C+B">B. Diemer</a>, <a href="/search/astro-ph?searchtype=author&query=Drake%2C+J">J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Meibody%2C+R+E">R. Emami Meibody</a>, <a href="/search/astro-ph?searchtype=author&query=Farah%2C+J+R">J. R. Farah</a>, <a href="/search/astro-ph?searchtype=author&query=Fazio%2C+G+G">G. G. Fazio</a>, <a href="/search/astro-ph?searchtype=author&query=Feigelson%2C+E">E. Feigelson</a>, <a href="/search/astro-ph?searchtype=author&query=Fornasini%2C+F">F. Fornasini</a>, <a href="/search/astro-ph?searchtype=author&query=Gallagher%2C+J">Jay Gallagher</a>, <a href="/search/astro-ph?searchtype=author&query=Grindlay%2C+J">J. Grindlay</a>, <a href="/search/astro-ph?searchtype=author&query=Hernquist%2C+L">L. Hernquist</a>, <a href="/search/astro-ph?searchtype=author&query=James%2C+D+J">D. J. James</a>, <a href="/search/astro-ph?searchtype=author&query=Karovska%2C+M">M. Karovska</a>, <a href="/search/astro-ph?searchtype=author&query=Kashyap%2C+V">V. Kashyap</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D+-">D. -W. Kim</a> , et al. (24 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="1903.06634v2-abstract-short" style="display: inline;"> We write in response to the call from the 2020 Decadal Survey to submit white papers illustrating the most pressing scientific questions in astrophysics for the coming decade. We propose exploration as the central question for the Decadal Committee's discussions.The history of astronomy shows that paradigm changing discoveries are not driven by well formulated scientific questions, based on the kn… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.06634v2-abstract-full').style.display = 'inline'; document.getElementById('1903.06634v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.06634v2-abstract-full" style="display: none;"> We write in response to the call from the 2020 Decadal Survey to submit white papers illustrating the most pressing scientific questions in astrophysics for the coming decade. We propose exploration as the central question for the Decadal Committee's discussions.The history of astronomy shows that paradigm changing discoveries are not driven by well formulated scientific questions, based on the knowledge of the time. They were instead the result of the increase in discovery space fostered by new telescopes and instruments. An additional tool for increasing the discovery space is provided by the analysis and mining of the increasingly larger amount of archival data available to astronomers. Revolutionary observing facilities, and the state of the art astronomy archives needed to support these facilities, will open up the universe to new discovery. Here we focus on exploration for compact objects and multi messenger science. This white paper includes science examples of the power of the discovery approach, encompassing all the areas of astrophysics covered by the 2020 Decadal Survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.06634v2-abstract-full').style.display = 'none'; document.getElementById('1903.06634v2-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 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.02574">arXiv:1903.02574</a> <span> [<a href="https://arxiv.org/pdf/1903.02574">pdf</a>, <a href="https://arxiv.org/format/1903.02574">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> X-rays Studies of the Solar System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Snios%2C+B">Bradford Snios</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+W+R">William R. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Lisse%2C+C+M">Carey M. Lisse</a>, <a href="/search/astro-ph?searchtype=author&query=Branduardi-Raymont%2C+G">Graziella Branduardi-Raymont</a>, <a href="/search/astro-ph?searchtype=author&query=Dennerl%2C+K">Konrad Dennerl</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+A">Anil Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Gladstone%2C+G+R">G. Randall Gladstone</a>, <a href="/search/astro-ph?searchtype=author&query=Nulsen%2C+S">Susan Nulsen</a>, <a href="/search/astro-ph?searchtype=author&query=Bodewits%2C+D">Dennis Bodewits</a>, <a href="/search/astro-ph?searchtype=author&query=Jackman%2C+C+M">Caitriona M. Jackman</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarado-G%C3%B3mez%2C+J+D">Juli谩n D. Alvarado-G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Bunce%2C+E+J">Emma J. Bunce</a>, <a href="/search/astro-ph?searchtype=author&query=Combi%2C+M+R">Michael R. Combi</a>, <a href="/search/astro-ph?searchtype=author&query=Cravens%2C+T+E">Thomas E. Cravens</a>, <a href="/search/astro-ph?searchtype=author&query=Cumbee%2C+R+S">Renata S. Cumbee</a>, <a href="/search/astro-ph?searchtype=author&query=Drake%2C+J+J">Jeremy J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Elsner%2C+R+F">Ronald F. Elsner</a>, <a href="/search/astro-ph?searchtype=author&query=Grodent%2C+D">Denis Grodent</a>, <a href="/search/astro-ph?searchtype=author&query=Hong%2C+J+S">Jae Sub Hong</a>, <a href="/search/astro-ph?searchtype=author&query=Kharchenko%2C+V">Vasili Kharchenko</a>, <a href="/search/astro-ph?searchtype=author&query=Kraft%2C+R+P">Ralph P. Kraft</a>, <a href="/search/astro-ph?searchtype=author&query=Marler%2C+J+P">Joan P. Marler</a>, <a href="/search/astro-ph?searchtype=author&query=Moschou%2C+S+P">Sofia P. Moschou</a>, <a href="/search/astro-ph?searchtype=author&query=Mullen%2C+P+D">Patrick D. Mullen</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</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="1903.02574v1-abstract-short" style="display: inline;"> X-ray observatories contribute fundamental advances in Solar System studies by probing Sun-object interactions, developing planet and satellite surface composition maps, probing global magnetospheric dynamics, and tracking astrochemical reactions. Despite these crucial results, the technological limitations of current X-ray instruments hinder the overall scope and impact for broader scientific app… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.02574v1-abstract-full').style.display = 'inline'; document.getElementById('1903.02574v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.02574v1-abstract-full" style="display: none;"> X-ray observatories contribute fundamental advances in Solar System studies by probing Sun-object interactions, developing planet and satellite surface composition maps, probing global magnetospheric dynamics, and tracking astrochemical reactions. Despite these crucial results, the technological limitations of current X-ray instruments hinder the overall scope and impact for broader scientific application of X-ray observations both now and in the coming decade. Implementation of modern advances in X-ray optics will provide improvements in effective area, spatial resolution, and spectral resolution for future instruments. These improvements will usher in a truly transformative era of Solar System science through the study of X-ray emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.02574v1-abstract-full').style.display = 'none'; document.getElementById('1903.02574v1-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> 6 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">White paper submitted to Astro2020, the Astronomy and Astrophysics Decadal Survey</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.05525">arXiv:1901.05525</a> <span> [<a href="https://arxiv.org/pdf/1901.05525">pdf</a>, <a href="https://arxiv.org/format/1901.05525">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab7b5c">10.3847/1538-4357/ab7b5c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pointing Chandra Toward the Extreme Ultraviolet Fluxes of Very Low-Mass Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Drake%2C+J+J">Jeremy J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Kashyap%2C+V+L">Vinay L. Kashyap</a>, <a href="/search/astro-ph?searchtype=author&query=Wargelin%2C+B+J">Bradford J. Wargelin</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</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="1901.05525v1-abstract-short" style="display: inline;"> The X-ray and EUV emission of stars plays a key role in the loss and evolution of the atmospheres of their planets. The coronae of dwarf stars later than M6 appear to behave differently to those of earlier spectral types and are more X-ray dim and radio bright. Too faint to have been observed by the Extreme Ultraviolet Explorer, their EUV behavior is currently highly uncertain. We have devised a m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.05525v1-abstract-full').style.display = 'inline'; document.getElementById('1901.05525v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.05525v1-abstract-full" style="display: none;"> The X-ray and EUV emission of stars plays a key role in the loss and evolution of the atmospheres of their planets. The coronae of dwarf stars later than M6 appear to behave differently to those of earlier spectral types and are more X-ray dim and radio bright. Too faint to have been observed by the Extreme Ultraviolet Explorer, their EUV behavior is currently highly uncertain. We have devised a method to use the Chandra X-ray Observatory High Resolution Camera to provide a measure of EUV emission in the 50-170 脜 range and have applied it to the M6.5 dwarf LHS 248 in a pilot 10 ks exposure. Analysis with model spectra using simple, idealised coronal emission measure distributions inspired by an analysis of Chandra HETG spectra of the M5.5 dwarf Proxima Cen and results from the literature, finds greatest consistency with a very shallow emission measure distribution slope, $DEM \propto T^{3/2}$ or shallower, in the range $\log T=5.5$-$6.5$. Within $2蟽$ confidence, a much wider range of slopes can be accommodated. Model spectra constrained by this method can provide accurate (within a factor of 2-4) synthesis and extrapolation of EUV spectra for wavelengths $<400$-500 脜. At longer wavelengths models are uncertain by an order of magnitude or more, and depend on the details of the emission measure distribution at temperatures $\log T < 5.5$. The method is sensitive to possible incompleteness of plasma radiative loss models in the 30 170 脜 range for which re-examination would be warranted. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.05525v1-abstract-full').style.display = 'none'; document.getElementById('1901.05525v1-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">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/1811.04505">arXiv:1811.04505</a> <span> [<a href="https://arxiv.org/pdf/1811.04505">pdf</a>, <a href="https://arxiv.org/ps/1811.04505">ps</a>, <a href="https://arxiv.org/format/1811.04505">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aaf4c1">10.3847/1538-4357/aaf4c1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Dynamics, Structure, and Fate of a Young Cluster During Gas Dispersal: Hectoschelle, Chandra, Spitzer, and Gaia Observations of CepOB3b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Karnath%2C+N">N. Karnath</a>, <a href="/search/astro-ph?searchtype=author&query=Prchlik%2C+J+K">J. K. Prchlik</a>, <a href="/search/astro-ph?searchtype=author&query=Gutermuth%2C+R+A">R. A. Gutermuth</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+T+S">T. S. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Megeath%2C+S+T">S. T. Megeath</a>, <a href="/search/astro-ph?searchtype=author&query=Pipher%2C+J+L">J. L. Pipher</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S">S. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</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="1811.04505v1-abstract-short" style="display: inline;"> We present a study of the kinematics and structure of the Cep OB3b cluster based on new spectra obtained with the Hectoschelle spectrograph on the MMT and data from Spitzer, Chandr}, and Gaia. At a distance of 819+/-16 pc, Cep OB3b is one of the closest examples of a young (~3 - 5 Myr), large (~3000 total members) cluster at the late stages of gas dispersal. The cluster is broken into two sub-clus… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.04505v1-abstract-full').style.display = 'inline'; document.getElementById('1811.04505v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.04505v1-abstract-full" style="display: none;"> We present a study of the kinematics and structure of the Cep OB3b cluster based on new spectra obtained with the Hectoschelle spectrograph on the MMT and data from Spitzer, Chandr}, and Gaia. At a distance of 819+/-16 pc, Cep OB3b is one of the closest examples of a young (~3 - 5 Myr), large (~3000 total members) cluster at the late stages of gas dispersal. The cluster is broken into two sub-clusters surrounded by a lower density halo. We fit the empirical density law of King (1962) to each sub-cluster to constrain their sizes and structure. The richer eastern sub-cluster has circular symmetry, a modest central density, and lacks molecular gas toward its core suggesting it has undergone expansion due to gas dispersal. In contrast, the western sub-cluster deviates from circular symmetry, has a smaller core size, and contains significant molecular gas near its core, suggesting that it is in an earlier phase of gas dispersal. We present posterior probability distributions for the velocity dispersions from the Hectoschelle spectra. The east will continue to expand and likely form a bound cluster with ~35% of stars remaining. The west is undergoing slower gas dispersal and will potentially form a bound cluster with ~75% of stars remaining. If the halo dissipates, this will leave two independent clusters with ~300 members; proper motions suggest that the two sub-clusters are not bound to each other. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.04505v1-abstract-full').style.display = 'none'; document.getElementById('1811.04505v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">44 pages, 15 figures, 9 tables, accepted 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/1807.06995">arXiv:1807.06995</a> <span> [<a href="https://arxiv.org/pdf/1807.06995">pdf</a>, <a href="https://arxiv.org/format/1807.06995">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/aac9bd">10.3847/1538-3881/aac9bd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical dimming of RW Aur associated with an iron rich corona and exceptionally high absorbing column density </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+H+M">Hans Moritz G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Birnstiel%2C+T">T. Birnstiel</a>, <a href="/search/astro-ph?searchtype=author&query=Huenemoerder%2C+D+P">D. P. Huenemoerder</a>, <a href="/search/astro-ph?searchtype=author&query=Principe%2C+D+A">D. A. Principe</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+P+C">P. C. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">S. J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Dubois%2C+F">Franky Dubois</a>, <a href="/search/astro-ph?searchtype=author&query=Logie%2C+L">Ludwig Logie</a>, <a href="/search/astro-ph?searchtype=author&query=Rau%2C+S">Steve Rau</a>, <a href="/search/astro-ph?searchtype=author&query=Vanaverbeke%2C+S">Sigfried Vanaverbeke</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="1807.06995v1-abstract-short" style="display: inline;"> RW Aur is a binary system composed of two young, low-mass stars. The primary, RW Aur A, has undergone visual dimming events ($螖V =2-3$~mag) in 2011, 2014-16, and 2017-2018. Visual and IR observations indicate a gray absorber that moved into the line-of-sight. This dimming is also associated with changes in the outflow. In 2017, when the optical brightness was almost 2~mag below the long-term avera… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.06995v1-abstract-full').style.display = 'inline'; document.getElementById('1807.06995v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.06995v1-abstract-full" style="display: none;"> RW Aur is a binary system composed of two young, low-mass stars. The primary, RW Aur A, has undergone visual dimming events ($螖V =2-3$~mag) in 2011, 2014-16, and 2017-2018. Visual and IR observations indicate a gray absorber that moved into the line-of-sight. This dimming is also associated with changes in the outflow. In 2017, when the optical brightness was almost 2~mag below the long-term average we triggered a Chandra observation to measure the absorbing column density $N_\mathrm{H}$ and to constrain dust properties and the gas-to-dust ratio of the absorber. In 2017, the X-ray spectrum is more absorbed than it was in the optically bright state ($N_\mathrm{H} = (4\pm 1) \times 10^{23}\;\mathrm{cm}^{-2}$) and shows significantly more hot plasma than in X-ray observations taken before. Also, a new emission feature at $6.63\pm0.02$ keV (statistic) $\pm0.02$ keV (systematic) appeared indicating an Fe abundance an order of magnitude above Solar, in contrast with previous sub-Solar Fe abundance measurements. Comparing X-ray absorbing column density $N_\mathrm{H}$ and optical extinction $A_V$, we find that either the gas-to-dust ratio in the absorber is orders of magnitude higher than in the ISM or the absorber has undergone significant dust evolution. Given the high column density coupled with changes in the X-ray spectral shape, this absorber is probably located in the inner disk. We speculate that a break-up of planetesimals or a terrestrial planet could supply large grains causing gray absorption; some of these grains would be accreted and enrich the stellar corona with iron which could explain the inferred high abundance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.06995v1-abstract-full').style.display = 'none'; document.getElementById('1807.06995v1-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 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">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/1805.05489">arXiv:1805.05489</a> <span> [<a href="https://arxiv.org/pdf/1805.05489">pdf</a>, <a href="https://arxiv.org/format/1805.05489">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> <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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Science Impacts of the SPHEREx All-Sky Optical to Near-Infrared Spectral Survey II: Report of a Community Workshop on the Scientific Synergies Between the SPHEREx Survey and Other Astronomy Observatories </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dor%C3%A9%2C+O">Olivier Dor茅</a>, <a href="/search/astro-ph?searchtype=author&query=Werner%2C+M+W">Michael W. Werner</a>, <a href="/search/astro-ph?searchtype=author&query=Ashby%2C+M+L+N">Matthew L. N. Ashby</a>, <a href="/search/astro-ph?searchtype=author&query=Bleem%2C+L+E">Lindsey E. Bleem</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J">Jamie Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Burt%2C+J">Jennifer Burt</a>, <a href="/search/astro-ph?searchtype=author&query=Capak%2C+P">Peter Capak</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+T">Tzu-Ching Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chaves-Montero%2C+J">Jon谩s Chaves-Montero</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+C+H">Christine H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Civano%2C+F">Francesca Civano</a>, <a href="/search/astro-ph?searchtype=author&query=Cleeves%2C+I+I">I. Ilsedore Cleeves</a>, <a href="/search/astro-ph?searchtype=author&query=Cooray%2C+A">Asantha Cooray</a>, <a href="/search/astro-ph?searchtype=author&query=Crill%2C+B">Brendan Crill</a>, <a href="/search/astro-ph?searchtype=author&query=Crossfield%2C+I+J+M">Ian J. M. Crossfield</a>, <a href="/search/astro-ph?searchtype=author&query=Cushing%2C+M">Michael Cushing</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Torre%2C+S">Sylvain de la Torre</a>, <a href="/search/astro-ph?searchtype=author&query=DiMatteo%2C+T">Tiziana DiMatteo</a>, <a href="/search/astro-ph?searchtype=author&query=Dvory%2C+N">Niv Dvory</a>, <a href="/search/astro-ph?searchtype=author&query=Dvorkin%2C+C">Cora Dvorkin</a>, <a href="/search/astro-ph?searchtype=author&query=Espaillat%2C+C">Catherine Espaillat</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Finkbeiner%2C+D">Douglas Finkbeiner</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J">Jenny Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Hewitt%2C+J">Jackie Hewitt</a> , et al. (38 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="1805.05489v2-abstract-short" style="display: inline;"> SPHEREx is a proposed NASA MIDEX mission selected for Phase A study. SPHEREx would carry out the first all-sky spectral survey in the near infrared. At the end of its two-year mission, SPHEREx would obtain 0.75-to-5$渭$m spectra of every 6.2 arcsec pixel on the sky, with spectral resolution R>35 and a 5-$蟽$ sensitivity AB$>$19 per spectral/spatial resolution element. More details concerning SPHEREx… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.05489v2-abstract-full').style.display = 'inline'; document.getElementById('1805.05489v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.05489v2-abstract-full" style="display: none;"> SPHEREx is a proposed NASA MIDEX mission selected for Phase A study. SPHEREx would carry out the first all-sky spectral survey in the near infrared. At the end of its two-year mission, SPHEREx would obtain 0.75-to-5$渭$m spectra of every 6.2 arcsec pixel on the sky, with spectral resolution R>35 and a 5-$蟽$ sensitivity AB$>$19 per spectral/spatial resolution element. More details concerning SPHEREx are available at http://spherex.caltech.edu. The SPHEREx team has proposed three specific science investigations to be carried out with this unique data set: cosmic inflation, interstellar and circumstellar ices, and the extra-galactic background light. Though these three themes are undoubtedly compelling, they are far from exhausting the scientific output of SPHEREx. Indeed, SPHEREx would create a unique all-sky spectral database including spectra of very large numbers of astronomical and solar system targets, including both extended and diffuse sources. These spectra would enable a wide variety of investigations, and the SPHEREx team is dedicated to making the data available to the community to enable these investigations, which we refer to as Legacy Science. To that end, we have sponsored two workshops for the general scientific community to identify the most interesting Legacy Science themes and to ensure that the SPHEREx data products are responsive to their needs. In February of 2016, some 50 scientists from all fields met in Pasadena to develop these themes and to understand their implications for the SPHEREx mission. The 2016 workshop highlighted many synergies between SPHEREx and other contemporaneous astronomical missions, facilities, and databases. Consequently, in January 2018 we convened a second workshop at the Center for Astrophysics in Cambridge to focus specifically on these synergies. This white paper reports on the results of the 2018 SPHEREx workshop. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.05489v2-abstract-full').style.display = 'none'; document.getElementById('1805.05489v2-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 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 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">50 pages, 24 figures, more details at http://spherex.caltech.edu</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.05067">arXiv:1804.05067</a> <span> [<a href="https://arxiv.org/pdf/1804.05067">pdf</a>, <a href="https://arxiv.org/ps/1804.05067">ps</a>, <a href="https://arxiv.org/format/1804.05067">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/aabe82">10.3847/1538-3881/aabe82 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chandra Detection of An Evolved Population of Young Stars in Serpens South </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Winston%2C+E+M">Elaine M. Winston</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Gutermuth%2C+R">Robert Gutermuth</a>, <a href="/search/astro-ph?searchtype=author&query=Bourke%2C+T+L">Tyler L. Bourke</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="1804.05067v1-abstract-short" style="display: inline;"> We present a Chandra study of the deeply embedded Serpens South star-forming region, examining cluster structure and disk properties at the earliest stages. In total, 152 X-ray sources are detected. Combined with Spitzer and 2MASS photometry, 66 X-ray sources are reliably matched to an IR counterpart. We identify 21 class I, 6 flat spectrum, 16 class II, and 18 class III young stars; 5 were unclas… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.05067v1-abstract-full').style.display = 'inline'; document.getElementById('1804.05067v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.05067v1-abstract-full" style="display: none;"> We present a Chandra study of the deeply embedded Serpens South star-forming region, examining cluster structure and disk properties at the earliest stages. In total, 152 X-ray sources are detected. Combined with Spitzer and 2MASS photometry, 66 X-ray sources are reliably matched to an IR counterpart. We identify 21 class I, 6 flat spectrum, 16 class II, and 18 class III young stars; 5 were unclassified. Eighteen sources were variable in X-rays, 8 exhibiting flare-like emission, and one periodic source. The cluster X-ray luminosity distance was estimated, the best match was to the nearer distance of 260pc for the front of the Aquila Rift complex. The $N_{H}$ vs. $A_{K}$ ratio is found to be $\sim$0.68x10$^{22}$, similar to that measured in other young low mass regions, but lower than that measured in the ISM and high mass clusters ($\sim$1.6-2x10$^{22}$). We find the spatial distribution closely follows that of the dense filament from which the stars have formed, with the class II population still strongly associated with the filament. There are four sub-clusters in the field, with three forming knots in the filament, and a fourth to the west, which may not be associated but may be contributing to the distributed class III population. A high percentage of diskless class IIIs (upper limit 30% of classified X-ray sources) in such a young cluster could indicate that processing of disks is influenced by the cluster environment and is not solely time-scale dependent. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.05067v1-abstract-full').style.display = 'none'; document.getElementById('1804.05067v1-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 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">56 pages, 11 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1712.00728">arXiv:1712.00728</a> <span> [<a href="https://arxiv.org/pdf/1712.00728">pdf</a>, <a href="https://arxiv.org/format/1712.00728">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/10.1051/0004-6361/201732078">10.1051/0004-6361/201732078 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of magnetic field in the B2 star $蟻$ Oph A with ESO FORS2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriguez%2C+N+C">N. Castro Rodriguez</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L">L. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">S. J. Wolk</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="1712.00728v1-abstract-short" style="display: inline;"> Circumstantial evidence suggests that magnetism and enhanced X-ray emission are likely correlated in early B-type stars: similar fractions of them ($\sim$ 10 %) are strong and hard X-ray sources and possess strong magnetic fields. It is also known that some B-type stars have spots on their surface. Yet up to now no X-ray activity associated with spots on early-type stars was detected. In this Lett… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.00728v1-abstract-full').style.display = 'inline'; document.getElementById('1712.00728v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1712.00728v1-abstract-full" style="display: none;"> Circumstantial evidence suggests that magnetism and enhanced X-ray emission are likely correlated in early B-type stars: similar fractions of them ($\sim$ 10 %) are strong and hard X-ray sources and possess strong magnetic fields. It is also known that some B-type stars have spots on their surface. Yet up to now no X-ray activity associated with spots on early-type stars was detected. In this Letter we report the detection of a magnetic field on the B2V star $蟻$ Oph A. Previously, we assessed that the X-ray activity of this star is associated with a surface spot, herewith we establish its magnetic origin. We analyzed FORS2 ESO VLT spectra of $蟻$ Oph A taken at two epochs and detected a longitudinal component of the magnetic field of order of $\sim500$ G in one of the datasets. The detection of the magnetic field only at one epoch can be explained by stellar rotation which is also invoked to explain observed periodic X-ray activity. From archival HARPS ESO VLT high resolution spectra we derived the fundamental stellar parameters of $蟻$ Oph A and further constrained its age. We conclude that $蟻$ Oph A provides strong evidence for the presence of active X-ray emitting regions on young magnetized early type stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.00728v1-abstract-full').style.display = 'none'; document.getElementById('1712.00728v1-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 December, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">4 pages, 1 figure, 2 tables, accepted as a "Letter to the Editor" 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 610, L3 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.04673">arXiv:1711.04673</a> <span> [<a href="https://arxiv.org/pdf/1711.04673">pdf</a>, <a href="https://arxiv.org/format/1711.04673">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201731303">10.1051/0004-6361/201731303 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> XMM-Newton imaging of V1818 Ori: a young stellar group on the eastern edge of the Kappa Ori ring </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">S. J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Megeath%2C+S+T">S. T. Megeath</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="1711.04673v1-abstract-short" style="display: inline;"> We present the results of a 40 ks XMM-Newton observation centered on the variable star V1818 Ori. Using a combination of the XMM-Newton and AllWISE catalog data, we identify a group of about 31 young stellar objects around V1818 Ori. This group is coincident with the eastern edge of the dust ring surrounding Kappa Ori. Previously, we concluded that the young stellar objects on the western side of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.04673v1-abstract-full').style.display = 'inline'; document.getElementById('1711.04673v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.04673v1-abstract-full" style="display: none;"> We present the results of a 40 ks XMM-Newton observation centered on the variable star V1818 Ori. Using a combination of the XMM-Newton and AllWISE catalog data, we identify a group of about 31 young stellar objects around V1818 Ori. This group is coincident with the eastern edge of the dust ring surrounding Kappa Ori. Previously, we concluded that the young stellar objects on the western side of ring were formed in an episode of star formation that started 3-5 Myr ago, and are at a distance similar to that of kappa Ori (250-280 pc) and in the foreground to the Orion A cloud. Here we use the XMM-Newton observation to calculate X-ray fluxes and luminosities of the young stars around V1818 Ori. We find that their X-ray luminosity function (XLF), calculated for a distance of ~270 pc, matches the XLF of the YSOs west of Kappa Ori. We rule out that this group of young stars is associated to Mon R2 as assumed in the literature, but rather they are part of the same Kappa Ori's ring stellar population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.04673v1-abstract-full').style.display = 'none'; document.getElementById('1711.04673v1-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 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">4 pages, 4 figures, 1 table. Accepted for publication to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 608, L2 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.08979">arXiv:1706.08979</a> <span> [<a href="https://arxiv.org/pdf/1706.08979">pdf</a>, <a href="https://arxiv.org/format/1706.08979">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div 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/stx1630">10.1093/mnras/stx1630 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Improved Age-Activity Relationship for Cool Stars older than a Gigayear </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Booth%2C+R+S">R. S. Booth</a>, <a href="/search/astro-ph?searchtype=author&query=Poppenhaeger%2C+K">K. Poppenhaeger</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+C+A">C. A. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre%2C+V+S">V. Silva Aguirre</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">S. J. Wolk</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="1706.08979v1-abstract-short" style="display: inline;"> Stars with convective envelopes display magnetic activity, which decreases over time due to the magnetic braking of the star. This age-dependence of magnetic activity is well-studied for younger stars, but the nature of this dependence for older stars is not well understood. This is mainly because absolute stellar ages for older stars are hard to measure. However, relatively accurate stellar ages… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.08979v1-abstract-full').style.display = 'inline'; document.getElementById('1706.08979v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.08979v1-abstract-full" style="display: none;"> Stars with convective envelopes display magnetic activity, which decreases over time due to the magnetic braking of the star. This age-dependence of magnetic activity is well-studied for younger stars, but the nature of this dependence for older stars is not well understood. This is mainly because absolute stellar ages for older stars are hard to measure. However, relatively accurate stellar ages have recently come into reach through asteroseismology. In this work we present X-ray luminosities, which are a measure for magnetic activity displayed by the stellar coronae, for 24 stars with well-determined ages older than a gigayear. We find 14 stars with detectable X-ray luminosities and use these to calibrate the age-activity relationship. We find a relationship between stellar X-ray luminosity, normalized by stellar surface area, and age that is steeper than the relationships found for younger stars, with an exponent of $-2.80 \pm 0.72$. Previous studies have found values for the exponent of the age-activity relationship ranging between -1.09 to -1.40, dependent on spectral type, for younger stars. Given that there are recent reports of a flattening relationship between age and rotational period for old cool stars, one possible explanation is that we witness a strong steepening of the relationship between activity and rotation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.08979v1-abstract-full').style.display = 'none'; document.getElementById('1706.08979v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">16 pages, 5 figures, 5 tables, Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.05562">arXiv:1706.05562</a> <span> [<a href="https://arxiv.org/pdf/1706.05562">pdf</a>, <a href="https://arxiv.org/ps/1706.05562">ps</a>, <a href="https://arxiv.org/format/1706.05562">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/aa7aa4">10.3847/1538-4357/aa7aa4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extreme radio flares and associated X-ray variability from young stellar objects in the Orion Nebula Cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Forbrich%2C+J">Jan Forbrich</a>, <a href="/search/astro-ph?searchtype=author&query=Reid%2C+M+J">Mark J. Reid</a>, <a href="/search/astro-ph?searchtype=author&query=Menten%2C+K+M">Karl M. Menten</a>, <a href="/search/astro-ph?searchtype=author&query=Rivilla%2C+V">Victor Rivilla</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Rau%2C+U">Urvashi Rau</a>, <a href="/search/astro-ph?searchtype=author&query=Chandler%2C+C+J">Claire J. Chandler</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="1706.05562v1-abstract-short" style="display: inline;"> Young stellar objects are known to exhibit strong radio variability on timescales of weeks to months, and a few reports have documented extreme radio flares, with at least an order of magnitude change in flux density on timescales of hours to days. However, there have been few constraints on the occurrence rate of such radio flares or on the correlation with pre-main sequence X-ray flares, althoug… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.05562v1-abstract-full').style.display = 'inline'; document.getElementById('1706.05562v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.05562v1-abstract-full" style="display: none;"> Young stellar objects are known to exhibit strong radio variability on timescales of weeks to months, and a few reports have documented extreme radio flares, with at least an order of magnitude change in flux density on timescales of hours to days. However, there have been few constraints on the occurrence rate of such radio flares or on the correlation with pre-main sequence X-ray flares, although such correlations are known for the Sun and nearby active stars. Here we report simultaneous deep VLA radio and Chandra X-ray observations of the Orion Nebula Cluster, targeting hundreds of sources to look for the occurrence rate of extreme radio variability and potential correlation with the most extreme X-ray variability. We identify 13 radio sources with extreme radio variability, with some showing an order of magnitude change in flux density in less than 30 minutes. All of these sources show X-ray emission and variability, but only on timescales <1h do we find clear correlations with extreme radio flaring. Strong X-ray variability does not predict the extreme radio sources and vice versa. Radio flares thus provide us with a new perspective on high-energy processes in YSOs and the irradiation of their protoplanetary disks. Finally, our results highlight implications for interferometric imaging of sources violating the constant-sky assumption. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.05562v1-abstract-full').style.display = 'none'; document.getElementById('1706.05562v1-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">18 pages, 13 sources, 7 figures. ApJ, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.04686">arXiv:1703.04686</a> <span> [<a href="https://arxiv.org/pdf/1703.04686">pdf</a>, <a href="https://arxiv.org/format/1703.04686">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/201630070">10.1051/0004-6361/201630070 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The early B-type star Rho Oph A is an X-ray lighthouse </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">Ignazio Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Wolk%2C+S+J">Scott J. Wolk</a>, <a href="/search/astro-ph?searchtype=author&query=Reale%2C+F">Fabio Reale</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L">Lida Oskinova</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="1703.04686v2-abstract-short" style="display: inline;"> We present the results of a 140 ks XMM-Newton observation of the B2 star $蟻$ Ophiuchi A. The star has exhibited strong X-ray variability: a cusp-shaped increase of rate, similar to that which we partially observed in 2013, and a bright flare. These events are separated in time by about 104 ks, which likely corresponds to the rotational period of the star (1.2 days). Time resolved spectroscopy of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.04686v2-abstract-full').style.display = 'inline'; document.getElementById('1703.04686v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.04686v2-abstract-full" style="display: none;"> We present the results of a 140 ks XMM-Newton observation of the B2 star $蟻$ Ophiuchi A. The star has exhibited strong X-ray variability: a cusp-shaped increase of rate, similar to that which we partially observed in 2013, and a bright flare. These events are separated in time by about 104 ks, which likely corresponds to the rotational period of the star (1.2 days). Time resolved spectroscopy of the X-ray spectra shows that the first event is caused by an increase of the plasma emission measure, while the second increase of rate is a major flare with temperatures in excess of 60 MK ($kT\sim5$ keV). From the analysis of its rise, we infer a magnetic field of $\ge300$ G and a size of the flaring region of $\sim1.4-1.9\times10^{11}$ cm, which corresponds to $\sim25\%-30\%$ of the stellar radius. We speculate that either an intrinsic magnetism that produces a hot spot on its surface or an unknown low mass companion are the source of such X-rays and variability. A hot spot of magnetic origin should be a stable structure over a time span of $\ge$2.5 years, and suggests an overall large scale dipolar magnetic field that produces an extended feature on the stellar surface. In the second scenario, a low mass unknown companion is the emitter of X-rays and it should orbit extremely close to the surface of the primary in a locked spin-orbit configuration, almost on the verge of collapsing onto the primary. As such, the X-ray activity of the secondary star would be enhanced by its young age, and the tight orbit as in RS Cvn systems and $蟻$ Ophiuchi would constitute an extreme system that is worthy of further investigation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.04686v2-abstract-full').style.display = 'none'; document.getElementById('1703.04686v2-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">10 pages, 7 figures, 2 tables, A&A accepted, this is the version after the language editor corrections</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Wolk%2C+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Wolk%2C+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Wolk%2C+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Wolk%2C+S&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Wolk%2C+S&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" 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