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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.04572">arXiv:2306.04572</a> <span> [<a href="https://arxiv.org/pdf/2306.04572">pdf</a>, <a href="https://arxiv.org/format/2306.04572">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1538-3873/acd7a3">10.1088/1538-3873/acd7a3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Near Infrared Imager and Slitless Spectrograph for the James Webb Space Telescope -- III. Single Object Slitless Spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albert%2C+L">Loic Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Lafreniere%2C+D">David Lafreniere</a>, <a href="/search/astro-ph?searchtype=author&query=Doyon%2C+R">Rene Doyon</a>, <a href="/search/astro-ph?searchtype=author&query=Artigau%2C+E">Etienne Artigau</a>, <a href="/search/astro-ph?searchtype=author&query=Volk%2C+K">Kevin Volk</a>, <a href="/search/astro-ph?searchtype=author&query=Goudfrooij%2C+P">Paul Goudfrooij</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Radica%2C+M">Michael Radica</a>, <a href="/search/astro-ph?searchtype=author&query=Rowe%2C+J">Jason Rowe</a>, <a href="/search/astro-ph?searchtype=author&query=Espinoza%2C+N">Nestor Espinoza</a>, <a href="/search/astro-ph?searchtype=author&query=Roy%2C+A">Arpita Roy</a>, <a href="/search/astro-ph?searchtype=author&query=Filippazzo%2C+J+C">Joseph C. Filippazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Darveau-Bernier%2C+A">Antoine Darveau-Bernier</a>, <a href="/search/astro-ph?searchtype=author&query=Talens%2C+G+J">Geert Jan Talens</a>, <a href="/search/astro-ph?searchtype=author&query=Sivaramakrishnan%2C+A">Anand Sivaramakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Willott%2C+C+J">Chris J. Willott</a>, <a href="/search/astro-ph?searchtype=author&query=Fullerton%2C+A+W">Alexander W. Fullerton</a>, <a href="/search/astro-ph?searchtype=author&query=LaMassa%2C+S">Stephanie LaMassa</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchings%2C+J+B">John B. Hutchings</a>, <a href="/search/astro-ph?searchtype=author&query=Rowlands%2C+N">Neil Rowlands</a>, <a href="/search/astro-ph?searchtype=author&query=Vila%2C+M+B">M. Begona Vila</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+J">Julia Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Aldridge%2C+D">David Aldridge</a>, <a href="/search/astro-ph?searchtype=author&query=Maszkiewicz%2C+M">Michael Maszkiewicz</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+M">Mathilde Beaulieu</a> , et al. (15 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="2306.04572v1-abstract-short" style="display: inline;"> The Near Infrared Imager and Slitless Spectrograph instrument (NIRISS) is the Canadian Space Agency (CSA) contribution to the suite of four science instruments of JWST. As one of the three NIRISS observing modes, the Single Object Slitless Spectroscopy (SOSS) mode is tailor-made to undertake time-series observations of exoplanets to perform transit spectroscopy. The SOSS permits observing point so… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04572v1-abstract-full').style.display = 'inline'; document.getElementById('2306.04572v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.04572v1-abstract-full" style="display: none;"> The Near Infrared Imager and Slitless Spectrograph instrument (NIRISS) is the Canadian Space Agency (CSA) contribution to the suite of four science instruments of JWST. As one of the three NIRISS observing modes, the Single Object Slitless Spectroscopy (SOSS) mode is tailor-made to undertake time-series observations of exoplanets to perform transit spectroscopy. The SOSS permits observing point sources between 0.6 and 2.8 um at a resolving power of 650 at 1.25 um using a slit-less cross-dispersing grism while its defocussing cylindrical lens enables observing targets as bright as J=6.7 by spreading light across 23 pixels along the cross-dispersion axis. This paper officially presents the design of the SOSS mode, its operation, characterization, and its performance, from ground-based testing and flight-based Commissioning. On-sky measurements demonstrate a peak photon conversion efficiency of 55% at 1.2 um. The first time-series on the A-type star BD+60o1753 achieves a flux stability close to the photon-noise limit, so far tested to a level of 20 parts per million on 40-minute time-scales after simply subtracting a long-term trend. Uncorrected 1/f noise residuals underneath the spectral traces add an extra source of noise equivalent to doubling the readout noise. Preliminary analysis of a HAT-P-14b transit time-series indicates that it is difficult to remove all the noise in pixels with partially saturated ramps. Overall, the SOSS delivers performance at the level required to tackle key exoplanet science programs such as detecting secondary atmospheres on terrestrial planets and measuring abundances of several chemical species in gas giants. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04572v1-abstract-full').style.display = 'none'; document.getElementById('2306.04572v1-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 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">41 pages, 28 figures, accepted for publication in PASP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.03277">arXiv:2306.03277</a> <span> [<a href="https://arxiv.org/pdf/2306.03277">pdf</a>, <a href="https://arxiv.org/format/2306.03277">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"> The Near Infrared Imager and Slitless Spectrograph for the James Webb Space Telescope -- I. Instrument Overview and in-Flight Performance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Doyon%2C+R">Rene Doyon</a>, <a href="/search/astro-ph?searchtype=author&query=Willott%2C+C+J">C. J Willott</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchings%2C+J+B">John B. Hutchings</a>, <a href="/search/astro-ph?searchtype=author&query=Sivaramakrishnan%2C+A">Anand Sivaramakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+L">Loic Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Lafreniere%2C+D">David Lafreniere</a>, <a href="/search/astro-ph?searchtype=author&query=Rowlands%2C+N">Neil Rowlands</a>, <a href="/search/astro-ph?searchtype=author&query=Vila%2C+M+B">M. Begona Vila</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=LaMassa%2C+S">Stephanie LaMassa</a>, <a href="/search/astro-ph?searchtype=author&query=Aldridge%2C+D">David Aldridge</a>, <a href="/search/astro-ph?searchtype=author&query=Artigau%2C+E">Etienne Artigau</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+P">Peter Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Chayer%2C+P">Pierre Chayer</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+N+J">Neil J. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+R+A">Rachel A. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Darveau-Bernier%2C+A">Antoine Darveau-Bernier</a>, <a href="/search/astro-ph?searchtype=author&query=Dupuis%2C+J">Jean Dupuis</a>, <a href="/search/astro-ph?searchtype=author&query=Earnshaw%2C+C">Colin Earnshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Espinoza%2C+N">Nestor Espinoza</a>, <a href="/search/astro-ph?searchtype=author&query=Filippazzo%2C+J+C">Joseph C. Filippazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Fullerton%2C+A+W">Alexander W. Fullerton</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudreau%2C+D">Daniel Gaudreau</a>, <a href="/search/astro-ph?searchtype=author&query=Gawlik%2C+R">Roman Gawlik</a>, <a href="/search/astro-ph?searchtype=author&query=Goudfrooij%2C+P">Paul Goudfrooij</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="2306.03277v1-abstract-short" style="display: inline;"> The Near-Infrared Imager and Slitless Spectrograph (NIRISS) is the science module of the Canadian-built Fine Guidance Sensor (FGS) onboard the James Webb Space Telescope (JWST). NIRISS has four observing modes: 1) broadband imaging featuring seven of the eight NIRCam broadband filters, 2) wide-field slitless spectroscopy (WFSS) at a resolving power of $\sim$150 between 0.8 and 2.2 $渭$m, 3) single-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.03277v1-abstract-full').style.display = 'inline'; document.getElementById('2306.03277v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.03277v1-abstract-full" style="display: none;"> The Near-Infrared Imager and Slitless Spectrograph (NIRISS) is the science module of the Canadian-built Fine Guidance Sensor (FGS) onboard the James Webb Space Telescope (JWST). NIRISS has four observing modes: 1) broadband imaging featuring seven of the eight NIRCam broadband filters, 2) wide-field slitless spectroscopy (WFSS) at a resolving power of $\sim$150 between 0.8 and 2.2 $渭$m, 3) single-object cross-dispersed slitless spectroscopy (SOSS) enabling simultaneous wavelength coverage between 0.6 and 2.8 $渭$m at R$\sim$700, a mode optimized for exoplanet spectroscopy of relatively bright ($J<6.3$) stars and 4) aperture masking interferometry (AMI) between 2.8 and 4.8 $渭$m enabling high-contrast ($\sim10^{-3}-10^{-4}$) imaging at angular separations between 70 and 400 milliarcsec for relatively bright ($M<8$) sources. This paper presents an overview of the NIRISS instrument, its design, its scientific capabilities, and a summary of in-flight performance. NIRISS shows significantly better response shortward of $\sim2.5\,渭$m resulting in 10-40% sensitivity improvement for broadband and low-resolution spectroscopy compared to pre-flight predictions. Two time-series observations performed during instrument commissioning in the SOSS mode yield very stable spectro-photometry performance within $\sim$10% of the expected noise. The first space-based companion detection of the tight binary star AB Dor AC through AMI was demonstrated. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.03277v1-abstract-full').style.display = 'none'; document.getElementById('2306.03277v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.04869">arXiv:2304.04869</a> <span> [<a href="https://arxiv.org/pdf/2304.04869">pdf</a>, <a href="https://arxiv.org/format/2304.04869">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1538-3873/acd1b5">10.1088/1538-3873/acd1b5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The James Webb Space Telescope Mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gardner%2C+J+P">Jonathan P. Gardner</a>, <a href="/search/astro-ph?searchtype=author&query=Mather%2C+J+C">John C. Mather</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">Randy Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abell%2C+J+S">James S. Abell</a>, <a href="/search/astro-ph?searchtype=author&query=Abernathy%2C+M">Mark Abernathy</a>, <a href="/search/astro-ph?searchtype=author&query=Abney%2C+F+E">Faith E. Abney</a>, <a href="/search/astro-ph?searchtype=author&query=Abraham%2C+J+G">John G. Abraham</a>, <a href="/search/astro-ph?searchtype=author&query=Abraham%2C+R">Roberto Abraham</a>, <a href="/search/astro-ph?searchtype=author&query=Abul-Huda%2C+Y+M">Yasin M. Abul-Huda</a>, <a href="/search/astro-ph?searchtype=author&query=Acton%2C+S">Scott Acton</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+K">Cynthia K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E">Evan Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adler%2C+D+S">David S. Adler</a>, <a href="/search/astro-ph?searchtype=author&query=Adriaensen%2C+M">Maarten Adriaensen</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">Jonathan Albert Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+M">Mansoor Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+N+S">Nasif S. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+T">Tanjira Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Albat%2C+R">R眉deger Albat</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+L">Lo茂c Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alberts%2C+S">Stacey Alberts</a>, <a href="/search/astro-ph?searchtype=author&query=Aldridge%2C+D">David Aldridge</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+M+M">Mary Marsha Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+S+S">Shaune S. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Altenburg%2C+M">Martin Altenburg</a> , et al. (983 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.04869v1-abstract-short" style="display: inline;"> Twenty-six years ago a small committee report, building on earlier studies, expounded a compelling and poetic vision for the future of astronomy, calling for an infrared-optimized space telescope with an aperture of at least $4m$. With the support of their governments in the US, Europe, and Canada, 20,000 people realized that vision as the $6.5m$ James Webb Space Telescope. A generation of astrono… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.04869v1-abstract-full').style.display = 'inline'; document.getElementById('2304.04869v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.04869v1-abstract-full" style="display: none;"> Twenty-six years ago a small committee report, building on earlier studies, expounded a compelling and poetic vision for the future of astronomy, calling for an infrared-optimized space telescope with an aperture of at least $4m$. With the support of their governments in the US, Europe, and Canada, 20,000 people realized that vision as the $6.5m$ James Webb Space Telescope. A generation of astronomers will celebrate their accomplishments for the life of the mission, potentially as long as 20 years, and beyond. This report and the scientific discoveries that follow are extended thank-you notes to the 20,000 team members. The telescope is working perfectly, with much better image quality than expected. In this and accompanying papers, we give a brief history, describe the observatory, outline its objectives and current observing program, and discuss the inventions and people who made it possible. We cite detailed reports on the design and the measured performance on orbit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.04869v1-abstract-full').style.display = 'none'; document.getElementById('2304.04869v1-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, 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">Accepted by PASP for the special issue on The James Webb Space Telescope Overview, 29 pages, 4 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/2210.17434">arXiv:2210.17434</a> <span> [<a href="https://arxiv.org/pdf/2210.17434">pdf</a>, <a href="https://arxiv.org/format/2210.17434">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1538-3873/acaebd">10.1088/1538-3873/acaebd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Near Infrared Imager and Slitless Spectrograph for the James Webb Space Telescope -- IV. Aperture Masking Interferometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sivaramakrishnan%2C+A">Anand Sivaramakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Tuthill%2C+P">Peter Tuthill</a>, <a href="/search/astro-ph?searchtype=author&query=Lloyd%2C+J+P">James P. Lloyd</a>, <a href="/search/astro-ph?searchtype=author&query=Greenbaum%2C+A+Z">Alexandra Z. Greenbaum</a>, <a href="/search/astro-ph?searchtype=author&query=Thatte%2C+D">Deepashri Thatte</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+R+A">Rachel A. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Vandal%2C+T">Thomas Vandal</a>, <a href="/search/astro-ph?searchtype=author&query=Kammerer%2C+J">Jens Kammerer</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Bermudez%2C+J">Joel Sanchez-Bermudez</a>, <a href="/search/astro-ph?searchtype=author&query=Pope%2C+B+J+S">Benjamin J. S. Pope</a>, <a href="/search/astro-ph?searchtype=author&query=Blakely%2C+D">Dori Blakely</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+L">Lo茂c Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+N+J">Neil J. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Johnstone%2C+D">Doug Johnstone</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andr茅 R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Volk%2C+K">Kevin Volk</a>, <a href="/search/astro-ph?searchtype=author&query=Soulain%2C+A">Anthony Soulain</a>, <a href="/search/astro-ph?searchtype=author&query=Artigau%2C+%C3%89">脡tienne Artigau</a>, <a href="/search/astro-ph?searchtype=author&query=Lafreni%C3%A8re%2C+D">David Lafreni猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Willott%2C+C+J">Chris J. Willott</a>, <a href="/search/astro-ph?searchtype=author&query=Parmentier%2C+S">S茅bastien Parmentier</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+K+E+S">K. E. Saavik Ford</a>, <a href="/search/astro-ph?searchtype=author&query=McKernan%2C+B">Barry McKernan</a>, <a href="/search/astro-ph?searchtype=author&query=Vila%2C+M+B">M. Bego帽a Vila</a>, <a href="/search/astro-ph?searchtype=author&query=Rowlands%2C+N">Neil Rowlands</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="2210.17434v2-abstract-short" style="display: inline;"> The James Webb Space Telescope's Near Infrared Imager and Slitless Spectrograph (JWST-NIRISS) flies a 7-hole non-redundant mask (NRM), the first such interferometer in space, operating at 3-5 \micron~wavelengths, and a bright limit of $\simeq 4$ magnitudes in W2. We describe the NIRISS Aperture Masking Interferometry (AMI) mode to help potential observers understand its underlying principles, pres… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.17434v2-abstract-full').style.display = 'inline'; document.getElementById('2210.17434v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.17434v2-abstract-full" style="display: none;"> The James Webb Space Telescope's Near Infrared Imager and Slitless Spectrograph (JWST-NIRISS) flies a 7-hole non-redundant mask (NRM), the first such interferometer in space, operating at 3-5 \micron~wavelengths, and a bright limit of $\simeq 4$ magnitudes in W2. We describe the NIRISS Aperture Masking Interferometry (AMI) mode to help potential observers understand its underlying principles, present some sample science cases, explain its operational observing strategies, indicate how AMI proposals can be developed with data simulations, and how AMI data can be analyzed. We also present key results from commissioning AMI. Since the allied Kernel Phase Imaging (KPI) technique benefits from AMI operational strategies, we also cover NIRISS KPI methods and analysis techniques, including a new user-friendly KPI pipeline. The NIRISS KPI bright limit is $\simeq 8$ W2 magnitudes. AMI (and KPI) achieve an inner working angle of $\sim 70$ mas that is well inside the $\sim 400$ mas NIRCam inner working angle for its circular occulter coronagraphs at comparable wavelengths. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.17434v2-abstract-full').style.display = 'none'; document.getElementById('2210.17434v2-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 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">30 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1401.0545">arXiv:1401.0545</a> <span> [<a href="https://arxiv.org/pdf/1401.0545">pdf</a>, <a href="https://arxiv.org/format/1401.0545">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/783/2/73">10.1088/0004-637X/783/2/73 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> AGN and quasar science with aperture masking interferometry on the James Webb Space Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ford%2C+K+E+S">K. E. Saavik Ford</a>, <a href="/search/astro-ph?searchtype=author&query=McKernan%2C+B">Barry McKernan</a>, <a href="/search/astro-ph?searchtype=author&query=Sivaramakrishnan%2C+A">Anand Sivaramakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andr茅 R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A">Anton Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lafreni%C3%A8re%2C+D">David Lafreni猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Parmentier%2C+S">S茅bastien Parmentier</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="1401.0545v2-abstract-short" style="display: inline;"> Due to feedback from accretion onto supermassive black holes (SMBHs), Active Galactic Nuclei (AGNs) are believed to play a key role in LambdaCDM cosmology and galaxy formation. However, AGNs' extreme luminosities and the small angular size of their accretion flows create a challenging imaging problem. We show James Webb Space Telescope's Near Infrared Imager and Slitless Spectrograph (JWST-NIRISS)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.0545v2-abstract-full').style.display = 'inline'; document.getElementById('1401.0545v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.0545v2-abstract-full" style="display: none;"> Due to feedback from accretion onto supermassive black holes (SMBHs), Active Galactic Nuclei (AGNs) are believed to play a key role in LambdaCDM cosmology and galaxy formation. However, AGNs' extreme luminosities and the small angular size of their accretion flows create a challenging imaging problem. We show James Webb Space Telescope's Near Infrared Imager and Slitless Spectrograph (JWST-NIRISS) Aperture Masking Interferometry (AMI) mode will enable true imaging (i.e. without any requirement of prior assumptions on source geometry) at ~65 mas angular resolution at the centers of AGNs. This is advantageous for studying complex extended accretion flows around SMBHs, and in other areas of angular-resolution-limited astrophysics. By simulating data sequences incorporating expected sources of noise, we demonstrate that JWST-NIRISS AMI mode can map extended structure at a pixel-to-pixel contrast of ~10^{-2} around an L=7.5 point source, using short exposure times (minutes). Such images will test models of AGN feedback, fuelling and structure (complementary with ALMA observations), and are not currently supported by any ground-based IR interferometer or telescope. Binary point source contrast with NIRISS is ~10^{-4} (for observing binary nuclei in merging galaxies), significantly better than current ground-based optical or IR interferometry. JWST-NIRISS' seven-hole non-redundant mask has a throughput of 15%, and utilizes NIRISS' F277W (2.77\micron), F380M (3.8\micron), F430M (4.3\micron), and F480M (4.8\micron) filters. NIRISS' square pixels are 65mas per side, with a field of view ~2\arcmin x 2\arcmin. We also extrapolate our results to AGN science enabled by non-redundant masking on future 2.4m and 16m space telescopes working at long-UV to near-IR wavelengths. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.0545v2-abstract-full').style.display = 'none'; document.getElementById('1401.0545v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 March, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 17 figures, accepted to ApJ; Revised version fixes typo in section 2.1 (to reflect factor of 2 improvement); faster download for figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2014, ApJ, 783, 73 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1201.1031">arXiv:1201.1031</a> <span> [<a href="https://arxiv.org/pdf/1201.1031">pdf</a>, <a href="https://arxiv.org/ps/1201.1031">ps</a>, <a href="https://arxiv.org/format/1201.1031">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/746/1/88">10.1088/0004-637X/746/1/88 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical and IR Photometry of Globular Clusters in NGC1399: Evidence for Color-Metallicity Nonlinearity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cho%2C+H">Hyejeon Cho</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Jordan%2C+A">Andres Jordan</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre R. Martel</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="1201.1031v1-abstract-short" style="display: inline;"> We combine new Wide Field Camera~3 IR Channel (WFC3/IR) F160W (H) imaging data for NGC1399, the central galaxy in the Fornax cluster, with archival F475W (g), F606W (V), F814W (I), and F850LP (z) optical data from the Advanced Camera for Surveys (ACS). The purely optical g-I, V-I, and g-z colors of NGC1399's rich globular cluster (GC) system exhibit clear bimodality, at least for magnitudes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.1031v1-abstract-full').style.display = 'inline'; document.getElementById('1201.1031v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1201.1031v1-abstract-full" style="display: none;"> We combine new Wide Field Camera~3 IR Channel (WFC3/IR) F160W (H) imaging data for NGC1399, the central galaxy in the Fornax cluster, with archival F475W (g), F606W (V), F814W (I), and F850LP (z) optical data from the Advanced Camera for Surveys (ACS). The purely optical g-I, V-I, and g-z colors of NGC1399's rich globular cluster (GC) system exhibit clear bimodality, at least for magnitudes $I_814 > 21.5$. The optical-IR I-H color distribution appears unimodal, and this impression is confirmed by mixture modeling analysis. The V-H colors show marginal evidence for bimodality, consistent with bimodality in V-I and unimodality in I-H. If bimodality is imposed for I-H with a double Gaussian model, the preferred blue/red split differs from that for optical colors; these "differing bimodalities" mean that the optical and optical-IR colors cannot both be linearly proportional to metallicity. Consistent with the differing color distributions, the dependence of I-H on g-I for the matched GC sample is significantly nonlinear, with an inflection point near the trough in the g-I color distribution; the result is similar for the I-H dependence on g-z colors taken from the ACS Fornax Cluster Survey. These g-z colors have been calibrated empirically against metallicity; applying this calibration yields a continuous, skewed, but single-peaked metallicity distribution. Taken together, these results indicate that nonlinear color-metallicity relations play an important role in shaping the observed bimodal distributions of optical colors in extragalactic GC systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.1031v1-abstract-full').style.display = 'none'; document.getElementById('1201.1031v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2012. </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, 12 figures, 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/0710.5560">arXiv:0710.5560</a> <span> [<a href="https://arxiv.org/pdf/0710.5560">pdf</a>, <a href="https://arxiv.org/ps/0710.5560">ps</a>, <a href="https://arxiv.org/format/0710.5560">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/524849">10.1086/524849 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Principal Component Analysis of the Time- and Position-Dependent Point Spread Function of the Advanced Camera for Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jee%2C+M+J">M. J. Jee</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Sirianni%2C+M">M. Sirianni</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+R+L">R. L. White</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</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="0710.5560v1-abstract-short" style="display: inline;"> We describe the time- and position-dependent point spread function (PSF) variation of the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS) with the principal component analysis (PCA) technique. The time-dependent change is caused by the temporal variation of the $HST$ focus whereas the position-dependent PSF variation in ACS/WFC at a given focus is mainly the result of changes i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0710.5560v1-abstract-full').style.display = 'inline'; document.getElementById('0710.5560v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0710.5560v1-abstract-full" style="display: none;"> We describe the time- and position-dependent point spread function (PSF) variation of the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS) with the principal component analysis (PCA) technique. The time-dependent change is caused by the temporal variation of the $HST$ focus whereas the position-dependent PSF variation in ACS/WFC at a given focus is mainly the result of changes in aberrations and charge diffusion across the detector, which appear as position-dependent changes in elongation of the astigmatic core and blurring of the PSF, respectively. Using >400 archival images of star cluster fields, we construct a ACS PSF library covering diverse environments of the $HST$ observations (e.g., focus values). We find that interpolation of a small number ($\sim20$) of principal components or ``eigen-PSFs'' per exposure can robustly reproduce the observed variation of the ellipticity and size of the PSF. Our primary interest in this investigation is the application of this PSF library to precision weak-lensing analyses, where accurate knowledge of the instrument's PSF is crucial. However, the high-fidelity of the model judged from the nice agreement with observed PSFs suggests that the model is potentially also useful in other applications such as crowded field stellar photometry, galaxy profile fitting, AGN studies, etc., which similarly demand a fair knowledge of the PSFs at objects' locations. Our PSF models, applicable to any WFC image rectified with the Lanczos3 kernel, are publicly available. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0710.5560v1-abstract-full').style.display = 'none'; document.getElementById('0710.5560v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 October, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to PASP. To appear in December issue. Figures are degraded to meet the size limit. High-resolution version can be downloaded at http://acs.pha.jhu.edu/~mkjee/acs_psf/acspsf.pdf</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0705.2171">arXiv:0705.2171</a> <span> [<a href="https://arxiv.org/pdf/0705.2171">pdf</a>, <a href="https://arxiv.org/ps/0705.2171">ps</a>, <a href="https://arxiv.org/format/0705.2171">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/517498">10.1086/517498 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a Ringlike Dark Matter Structure in the Core of the Galaxy Cluster Cl 0024+17 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jee%2C+M+J">M. J. Jee</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+R+L">R. L. White</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D+A">D. A. Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G+R">G. R. Meurer</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Der+Wel%2C+A">A. Van Der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L+D">L. D. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Homeier%2C+N+L">N. L. Homeier</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Mei%2C+S">S. Mei</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="0705.2171v1-abstract-short" style="display: inline;"> We present a comprehensive mass reconstruction of the rich galaxy cluster Cl 0024+17 at z~0.4 from ACS data, unifying both strong- and weak-lensing constraints. The weak-lensing signal from a dense distribution of background galaxies (~120 per square arcmin) across the cluster enables the derivation of a high-resolution parameter-free mass map. The strongly-lensed objects tightly constrain the m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0705.2171v1-abstract-full').style.display = 'inline'; document.getElementById('0705.2171v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0705.2171v1-abstract-full" style="display: none;"> We present a comprehensive mass reconstruction of the rich galaxy cluster Cl 0024+17 at z~0.4 from ACS data, unifying both strong- and weak-lensing constraints. The weak-lensing signal from a dense distribution of background galaxies (~120 per square arcmin) across the cluster enables the derivation of a high-resolution parameter-free mass map. The strongly-lensed objects tightly constrain the mass structure of the cluster inner region on an absolute scale, breaking the mass-sheet degeneracy. The mass reconstruction of Cl 0024+17 obtained in such a way is remarkable. It reveals a ringlike dark matter substructure at r~75" surrounding a soft, dense core at r~50". We interpret this peculiar sub-structure as the result of a high-speed line-of-sight collision of two massive clusters 1-2 Gyr ago. Such an event is also indicated by the cluster velocity distribution. Our numerical simulation with purely collisionless particles demonstrates that such density ripples can arise by radially expanding, decelerating particles that originally comprised the pre-collision cores. Cl 0024+17 can be likened to the bullet cluster 1E0657-56, but viewed $along$ the collision axis at a much later epoch. In addition, we show that the long-standing mass discrepancy for Cl 0024+17 between X-ray and lensing can be resolved by treating the cluster X-ray emission as coming from a superposition of two X-ray systems. The cluster's unusual X-ray surface brightness profile that requires a two isothermal sphere description supports this hypothesis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0705.2171v1-abstract-full').style.display = 'none'; document.getElementById('0705.2171v1-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 May, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in the June 1 issue of The Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.661:728-749,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0611278">arXiv:astro-ph/0611278</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0611278">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0611278">ps</a>, <a href="https://arxiv.org/format/astro-ph/0611278">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/510722">10.1086/510722 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Robust Test of Evolution near the Tip of the Red Giant Branch and Missing Giants in NGC 2808 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sandquist%2C+E+L">Eric L. Sandquist</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andr茅 R. Martel</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="astro-ph/0611278v1-abstract-short" style="display: inline;"> We describe a new method for robustly testing theoretical predictions of red giant evolution near the tip of the giant branch. When theoretical cumulative luminosity functions are shifted to align the tip in I-band and normalized at a luminosity level slightly brighter than the red giant bump, virtually all dependence on age and composition (heavy elements and helium abundance) is eliminated. Wh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0611278v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0611278v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0611278v1-abstract-full" style="display: none;"> We describe a new method for robustly testing theoretical predictions of red giant evolution near the tip of the giant branch. When theoretical cumulative luminosity functions are shifted to align the tip in I-band and normalized at a luminosity level slightly brighter than the red giant bump, virtually all dependence on age and composition (heavy elements and helium abundance) is eliminated. While significant comparisons with observations require large samples of giant stars, such samples are available for some of the most massive Milky Way globular clusters. We present comparisons with the clusters NGC 2808 and M5, and find that NGC 2808 has a deficiency of bright giants (with a probability of less than about 3% that a more extreme distribution of giant stars would have happened by chance). We discuss the possibilities that underestimated neutrino losses or strong mass loss could be responsible for the deficit of giants. While we cannot rule out the neutrino hypothesis, it cannot explain the apparent agreement between the M5 observations and models. On the other hand, strong mass loss provides a potential link between the giant star observations and NGC 2808's unusually blue horizontal branch. If the mass loss hypothesis is true, there is likely a significant population of He white dwarfs that could be uncovered with slightly deeper UV observations of the cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0611278v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0611278v1-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 November, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2006. </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, 2 figures, uses emulateapj, accepted for ApJ Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.654:L65-L68,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0602292">arXiv:astro-ph/0602292</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0602292">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0602292">ps</a>, <a href="https://arxiv.org/format/astro-ph/0602292">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/503801">10.1086/503801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HST/ACS Multiband Coronagraphic Imaging of the Debris Disk around Beta Pictoris </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Krist%2C+J+E">J. E. Krist</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L+D">L. D. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R+A">R. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+C+J">C. J. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E+S">E. S. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Goto%2C+T">T. Goto</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Holden%2C+B+P">B. P. Holden</a>, <a href="/search/astro-ph?searchtype=author&query=Homeier%2C+N+L">N. L. Homeier</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">L. Infante</a> , et al. (18 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0602292v2-abstract-short" style="display: inline;"> (Abridged.) We present F435W (B), F606W (Broad V), and F814W (Broad I) coronagraphic images of the debris disk around Beta Pictoris obtained with HST's Advanced Camera for Surveys. We confirm that the previously reported warp in the inner disk is a distinct secondary disk inclined by ~5 deg from the main disk. The main disk's northeast extension is linear from 80 to 250 AU, but the southwest ext… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0602292v2-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0602292v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0602292v2-abstract-full" style="display: none;"> (Abridged.) We present F435W (B), F606W (Broad V), and F814W (Broad I) coronagraphic images of the debris disk around Beta Pictoris obtained with HST's Advanced Camera for Surveys. We confirm that the previously reported warp in the inner disk is a distinct secondary disk inclined by ~5 deg from the main disk. The main disk's northeast extension is linear from 80 to 250 AU, but the southwest extension is distinctly bowed with an amplitude of ~1 AU over the same region. Both extensions of the secondary disk appear linear, but not collinear, from 80 to 150 AU. Within ~120 AU of the star, the main disk is ~50% thinner than previously reported. The surface-brightness profiles along the spine of the main disk are fitted with four distinct radial power laws between 40 and 250 AU, while those of the secondary disk between 80 and 150 AU are fitted with single power laws. These discrepancies suggest that the two disks have different grain compositions or size distributions. The F606W/F435W and F814W/F435W flux ratios of the composite disk are nonuniform and asymmetric about both projected axes of the disk. Within ~120 AU, the m_F435W-m_F606W and m_F435W-m_F814W colors along the spine of the main disk are ~10% and ~20% redder, respectively, than those of Beta Pic. These colors increasingly redden beyond ~120 AU, becoming 25% and 40% redder, respectively, than the star at 250 AU. We compare the observed red colors within ~120 AU with the simulated colors of non-icy grains having a radial number density ~r^-3 and different compositions, porosities, and minimum grain sizes. The observed colors are consistent with those of compact or moderately porous grains of astronomical silicate and/or graphite with sizes >0.15-0.20 um, but the colors are inconsistent with the blue colors expected from grains with porosities >90%. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0602292v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0602292v2-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, 2006; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 February, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2006. </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 (including 21 figures and 4 tables) in EmulateApJ format, accepted for publication in The Astronomical Journal. Full-resolution figures and fully processed FITS images (with error maps) are available at http://acs.pha.jhu.edu/~dag/betapic Version 2: Added 4 references and some clarifying text. Basic facts and conclusions are unchanged</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0601327">arXiv:astro-ph/0601327</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0601327">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0601327">ps</a>, <a href="https://arxiv.org/format/astro-ph/0601327">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/499259">10.1086/499259 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evolution of the Color-Magnitude Relation in High-Redshift Clusters: Blue Early-Type Galaxies and Red Pairs in RDCS J0910+5422 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mei%2C+S">S. Mei</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Stanford%2C+S+A">S. A. Stanford</a>, <a href="/search/astro-ph?searchtype=author&query=Holden%2C+B+P">B. P. Holden</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Homeier%2C+N">N. Homeier</a>, <a href="/search/astro-ph?searchtype=author&query=Postman%2C+M">M. Postman</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Rettura%2C+A">A. Rettura</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H">H. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Ettori%2C+S">S. Ettori</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenhardt%2C+P">P. Eisenhardt</a>, <a href="/search/astro-ph?searchtype=author&query=team%2C+t+A+I">the ACS IDT team</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="astro-ph/0601327v1-abstract-short" style="display: inline;"> The color-magnitude relation has been determined for the RDCS J0910+5422 cluster of galaxies at redshift z = 1.106. Cluster members were selected from HST ACS images, combined with ground--based near--IR imaging and optical spectroscopy. The observed early--type color--magnitude relation (CMR) in (i_775 -z_850) versus z_850 shows intrinsic scatters in color of 0.042 +/- 0.010 mag and 0.044 +/- 0… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0601327v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0601327v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0601327v1-abstract-full" style="display: none;"> The color-magnitude relation has been determined for the RDCS J0910+5422 cluster of galaxies at redshift z = 1.106. Cluster members were selected from HST ACS images, combined with ground--based near--IR imaging and optical spectroscopy. The observed early--type color--magnitude relation (CMR) in (i_775 -z_850) versus z_850 shows intrinsic scatters in color of 0.042 +/- 0.010 mag and 0.044 +/- 0.020 mag for ellipticals and S0s, respectively. From the scatter about the CMR, a mean luminosity--weighted age t > 3.3 Gyr (z > 3) is derived for the elliptical galaxies. Strikingly, the S0 galaxies in RDCS J0910+5422 are systematically bluer in (i_775 - z_850) by 0.07 +/- 0.02 mag, with respect to the ellipticals. The ellipticity distribution as a function of color indicates that the face-on S0s in this particular cluster have likely been classified as elliptical. Thus, if anything, the offset in color between the elliptical and S0 populations may be even more significant. The color offset between S0 and E corresponds to an age difference of ~1 Gyr, for a single-burst solar metallicity model. A solar metallicity model with an exponential decay in star formation will reproduce the offset for an age of 3.5 Gyr, i.e. the S0s have evolved gradually from star forming progenitors. The early--type population in this cluster appears to be still forming. The blue early-type disk galaxies in RDCS J0910+5422 likely represent the direct progenitors of the more evolved S0s that follow the same red sequence as ellipticals in other clusters. Thirteen red galaxy pairs are observed and the galaxies associated in pairs constitute ~40% of the CMR galaxies in this cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0601327v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0601327v1-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, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2006. </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">ApJ, in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 639 (2006) 81-94 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0511734">arXiv:astro-ph/0511734</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0511734">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0511734">ps</a>, <a href="https://arxiv.org/format/astro-ph/0511734">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/500167">10.1086/500167 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Overdensity of Galaxies near the Most Distant Radio-Loud Quasar </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W">W. Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Overzier%2C+R">R. Overzier</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+R+L">R. L. White</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L+D">L. D. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Jee%2C+M+K">M. K. Jee</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Mei%2C+S">S. Mei</a>, <a href="/search/astro-ph?searchtype=author&query=Zirm%2C+A+W">A. W. Zirm</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R+A">R. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+C+J">C. J. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E+S">E. S. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</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="astro-ph/0511734v1-abstract-short" style="display: inline;"> A five square arcminute region around the luminous radio-loud quasar SDSS J0836+0054 (z=5.8) hosts a wealth of associated galaxies, characterized by very red (1.3 < i_775 - z_{850} < 2.0) color. The surface density of these z~5.8 candidates is approximately six times higher than the number expected from deep ACS fields. This is one of the highest galaxy overdensities at high redshifts, which may… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0511734v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0511734v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0511734v1-abstract-full" style="display: none;"> A five square arcminute region around the luminous radio-loud quasar SDSS J0836+0054 (z=5.8) hosts a wealth of associated galaxies, characterized by very red (1.3 < i_775 - z_{850} < 2.0) color. The surface density of these z~5.8 candidates is approximately six times higher than the number expected from deep ACS fields. This is one of the highest galaxy overdensities at high redshifts, which may develop into a group or cluster. We also find evidence for a substructure associated with one of the candidates. It has two very faint companion objects within two arcseconds, which are likely to merge. The finding supports the results of a recent simulation that luminous quasars at high redshifts lie on the most prominent dark-matter filaments and are surrounded by many fainter galaxies. The quasar activity from these regions may signal the buildup of a massive system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0511734v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0511734v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 November, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2005. </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">Four figures. The Astrophysical Journal: in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.640:574-578,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0509759">arXiv:astro-ph/0509759</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0509759">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0509759">ps</a>, <a href="https://arxiv.org/format/astro-ph/0509759">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/498344">10.1086/498344 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Morphological Demographics of galaxies in the ACS Hubble Ultra Deep Parallel Fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Menanteau%2C+F">Felipe Menanteau</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">Holland C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Motta%2C+V">Veronica Motta</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">Narciso Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">Leopoldo Infante</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="astro-ph/0509759v1-abstract-short" style="display: inline;"> We present a morphological analysis of distant field galaxies using the deep ACS images from the public parallel NICMOS observations of the Hubble Ultra Deep Field obtained in the F435W (B), F606W (V), F775W (i) and F850LP (z) filters. We morphologically segregate galaxies using a combination of visual classification and objective machine based selection. We use the Asymmetry (A) and Central Con… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0509759v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0509759v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0509759v1-abstract-full" style="display: none;"> We present a morphological analysis of distant field galaxies using the deep ACS images from the public parallel NICMOS observations of the Hubble Ultra Deep Field obtained in the F435W (B), F606W (V), F775W (i) and F850LP (z) filters. We morphologically segregate galaxies using a combination of visual classification and objective machine based selection. We use the Asymmetry (A) and Central Concentration (C) parameters to characterize galaxies up to z_AB<25mag. We take advantage of the multicolor dataset and estimate redshifts for our sample using the Bayesian photometric redshift (BPZ) which enables us to investigate the evolution of their morphological demographics with redshift. Using a template fitting model and a maximum likelihood approach, we compute the star-formation rate (SFR) for galaxies up to z~1.3 and its contributions from different morphological types. We report that spirals are the main providers to the total SFR. The E/S0s contribution flattens out at z~1 while the Irr/Pec populations continuously rise to match the spirals contribution at z~1.0. We use the i-z and V-i color-magnitude diagrams to constrain the galaxies' formation histories and find that E/S0s show both a population of luminous red galaxies in place at z~1.2 and a bluer and fainter population resembling those of Irr/Pec at similar redshifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0509759v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0509759v1-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 September, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2005. </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, 6 figures. Accepted for publication in the Astronomical Journal. Full resolution paper at: http://acs.pha.jhu.edu/~felipe/e-prints/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.J.131:208-215,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0509308">arXiv:astro-ph/0509308</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0509308">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0509308">ps</a>, <a href="https://arxiv.org/format/astro-ph/0509308">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/498234">10.1086/498234 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Clustering of Star-forming Galaxies Near a Radio Galaxy at z=5.2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Overzier%2C+R+A">Roderik A. Overzier</a>, <a href="/search/astro-ph?searchtype=author&query=Miley%2C+G+K">G. K. Miley</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Zirm%2C+A+W">A. W. Zirm</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Rottgering%2C+H+J+A">H. J. A. Rottgering</a>, <a href="/search/astro-ph?searchtype=author&query=Venemans%2C+B">B. Venemans</a>, <a href="/search/astro-ph?searchtype=author&query=IDT%2C+t+A">the ACS IDT</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="astro-ph/0509308v1-abstract-short" style="display: inline;"> We present HST/ACS observations of the most distant radio galaxy known, TN J0924-2201 at z=5.2. This radio galaxy has 6 spectroscopically confirmed Lya emitting companion galaxies, and appears to lie within an overdense region. The radio galaxy is marginally resolved in i_775 and z_850 showing continuum emission aligned with the radio axis, similar to what is observed for lower redshift radio ga… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0509308v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0509308v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0509308v1-abstract-full" style="display: none;"> We present HST/ACS observations of the most distant radio galaxy known, TN J0924-2201 at z=5.2. This radio galaxy has 6 spectroscopically confirmed Lya emitting companion galaxies, and appears to lie within an overdense region. The radio galaxy is marginally resolved in i_775 and z_850 showing continuum emission aligned with the radio axis, similar to what is observed for lower redshift radio galaxies. Both the half-light radius and the UV star formation rate are comparable to the typical values found for Lyman break galaxies at z~4-5. The Lya emitters are sub-L* galaxies, with deduced star formation rates of 1-10 Msun/yr. One of the Lya emitters is only detected in Lya. Based on the star formation rate of ~3 Msun/yr calculated from Lya, the lack of continuum emission could be explained if the galaxy is younger than ~2 Myr and is producing its first stars. Observations in V_606, i_775, and z_850 were used to identify additional Lyman break galaxies associated with this structure. In addition to the radio galaxy, there are 22 V-break (z~5) galaxies with z_850<26.5 (5sigma), two of which are also in the spectroscopic sample. We compare the surface density of 2/arcmin^2 to that of similarly selected V-dropouts extracted from GOODS and the UDF Parallel fields. We find evidence for an overdensity to very high confidence (>99%), based on a counts-in-cells analysis applied to the control field. The excess is suggestive of the V-break objects being associated with a forming cluster around the radio galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0509308v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0509308v1-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 September, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2005. </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 (15 figures). Accepted to ApJ. Full resolution version available at http://acs.pha.jhu.edu/science/papers/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.637:58-73,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0508222">arXiv:astro-ph/0508222</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0508222">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0508222">ps</a>, <a href="https://arxiv.org/format/astro-ph/0508222">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/497069">10.1086/497069 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HST/ACS Images of the GG Tauri Circumbinary Disk </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Krist%2C+J+E">J. E. Krist</a>, <a href="/search/astro-ph?searchtype=author&query=Stapelfeldt%2C+K+R">K. R. Stapelfeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</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="astro-ph/0508222v2-abstract-short" style="display: inline;"> Hubble Space Telescope Advanced Camera for Surveys images of the young binary GG Tauri and its circumbinary disk in V and I bandpasses were obtained in 2002 and are the most detailed of this system to date. The confirm features previously seen in the disk including: a "gap" apparently caused by shadowing from circumstellar material; an asymmetrical distribution of light about the line of sight o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0508222v2-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0508222v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0508222v2-abstract-full" style="display: none;"> Hubble Space Telescope Advanced Camera for Surveys images of the young binary GG Tauri and its circumbinary disk in V and I bandpasses were obtained in 2002 and are the most detailed of this system to date. The confirm features previously seen in the disk including: a "gap" apparently caused by shadowing from circumstellar material; an asymmetrical distribution of light about the line of sight on the near edge of the disk; enhanced brightness along the near edge of the disk due to forward scattering; and a compact reflection nebula near the secondary star. New features are seen in the ACS images: two short filaments along the disk; localized but strong variations in disk intensity ("gaplets"); and a "spur" or filament extending from the reflection nebulosity near the secondary. The back side of the disk is detected in the V band for the first time. The disk appears redder than the combined light from the stars, which may be explained by a varied distribution of grain sizes. The brightness asymmetries along the disk suggest that it is asymmetrically illuminated by the stars due to extinction by nonuniform circumstellar material or the illuminated surface of the disk is warped by tidal effects (or perhaps both). Localized, time-dependent brightness variations in the disk are also seen. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0508222v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0508222v2-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 August, 2005; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 August, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 7 figures, accepted for publication in the Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0507614">arXiv:astro-ph/0507614</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0507614">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0507614">ps</a>, <a href="https://arxiv.org/format/astro-ph/0507614">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/444553">10.1086/444553 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Photometric Performance and Calibration of the HST Advanced Camera For Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sirianni%2C+M">M. Sirianni</a>, <a href="/search/astro-ph?searchtype=author&query=Jee%2C+M+J">M. J. Jee</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G">G. Meurer</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marchi%2C+G">G. De Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Gilliland%2C+R">R. Gilliland</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Mack%2C+J">J. Mack</a>, <a href="/search/astro-ph?searchtype=author&query=McCann%2C+W+J">W. J. McCann</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="astro-ph/0507614v1-abstract-short" style="display: inline;"> We present the photometric calibration of the HST Advanced Camera for Surveys (ACS). We give here an overview of the performance and calibration of the 2 CCD cameras, the Wide Field Channel (WFC) and the High Resolution Channel (HRC), and a description of the best techniques for reducing ACS CCD data. On-orbit observations of spectrophotometric standard stars have been used to revise the pre-l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0507614v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0507614v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0507614v1-abstract-full" style="display: none;"> We present the photometric calibration of the HST Advanced Camera for Surveys (ACS). We give here an overview of the performance and calibration of the 2 CCD cameras, the Wide Field Channel (WFC) and the High Resolution Channel (HRC), and a description of the best techniques for reducing ACS CCD data. On-orbit observations of spectrophotometric standard stars have been used to revise the pre-launch estimate of the instrument response curves to best match predicted and observed count rates. Synthetic photometry has been used to determine zeropoints for all filters in 3 magnitude systems and to derive interstellar extinction values for the ACS photometric systems. Due to the CCD internal scattering of long wavelength photons, the width of the PSF increases significantly in the near-IR and the aperture correction for photometry with near-IR filters depends on the spectral energy distribution of the source. We provide encircled energy curves and a detailed recipe to correct for the latter effect. Transformations between the ACS photometric systems and the UBVRI and WFPC2 systems are presented. In general, two sets of transformations are available: 1 based on the observation of 2 star clusters; the other on synthetic photometry. We discuss the accuracy of these transformations and their sensitivity to details of the spectra being transformed. Initial signs of detector degradation due to the HST radiative environment are already visible. We discuss the impact on the data in terms of dark rate increase, charge transfer inefficiency, and hot pixel population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0507614v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0507614v1-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, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2005. </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">101 pages, 29 figures, 31 tables; PASP accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> ST ScI Eprint #1670 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Publ.Astron.Soc.Pac.117:1049-1112,2005 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0505610">arXiv:astro-ph/0505610</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0505610">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0505610">ps</a>, <a href="https://arxiv.org/format/astro-ph/0505610">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/431921">10.1086/431921 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Feedback and Brightest Cluster Galaxy Formation: ACS Observations of the Radio Galaxy TN J1338--1942 at z=4.1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zirm%2C+A+W">Andrew W. Zirm</a>, <a href="/search/astro-ph?searchtype=author&query=Overzier%2C+R+A">R. A. Overzier</a>, <a href="/search/astro-ph?searchtype=author&query=Miley%2C+G+K">G. K. Miley</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=De+Breuck%2C+C">C. De Breuck</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Homeier%2C+N">N. Homeier</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Rottgering%2C+H+J+A">H. J. A. Rottgering</a>, <a href="/search/astro-ph?searchtype=author&query=Venemans%2C+B">B. Venemans</a>, <a href="/search/astro-ph?searchtype=author&query=IDT%2C+t+A">the ACS IDT</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="astro-ph/0505610v1-abstract-short" style="display: inline;"> We present deep optical imaging of the z=4.1 radio galaxy TN J1338--1942 obtained using the ACS on-board HST. The radio galaxy is known to reside within a large galaxy overdensity (both in physical extent and density contrast). There is good evidence that this `protocluster' region is the progenitor of a present-day rich galaxy cluster. TN J1338 is the dominant galaxy in the protocluster, in ter… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0505610v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0505610v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0505610v1-abstract-full" style="display: none;"> We present deep optical imaging of the z=4.1 radio galaxy TN J1338--1942 obtained using the ACS on-board HST. The radio galaxy is known to reside within a large galaxy overdensity (both in physical extent and density contrast). There is good evidence that this `protocluster' region is the progenitor of a present-day rich galaxy cluster. TN J1338 is the dominant galaxy in the protocluster, in terms of size and luminosity and therefore seems destined to evolve into the brightest cluster galaxy. The high spatial-resolution ACS images reveal several kpc-scale features within and around the radio galaxy. The continuum light is aligned with the radio axis and is resolved into two clumps in the i-band and z-band bands. These components have luminosities ~10^9 L_sun and sizes of a few kpc. The estimated star-formation rate for the whole radio galaxy is ~200 M_sun/yr. A simple model in which the jet has triggered star-formation in these continuum knots is consistent with the available data. An unusual feature is seen in Lyman-alpha emission. A wedge-shaped extension emanates from the radio galaxy perpendicularly to the radio axis. This `wedge' naturally connects to the surrounding, asymmetric, large-scale (~100 kpc) Lyman-alpha halo. We posit that the wedge is a starburst-driven superwind, associated with the first major epoch of formation of the brightest cluster galaxy. The shock and wedge are examples of feedback processes due to both AGN and star-formation in the earliest stages of massive galaxy formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0505610v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0505610v1-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 May, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2005. </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, 12 figures. Accepted to ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 630 (2005) 68-81 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0503445">arXiv:astro-ph/0503445</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0503445">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0503445">ps</a>, <a href="https://arxiv.org/format/astro-ph/0503445">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/430395">10.1086/430395 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Dynamical Simulation of the Debris Disk Around HD 141569A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Lubow%2C+S+H">S. H. Lubow</a>, <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Krist%2C+J+E">J. E. Krist</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L+D">L. D. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R+A">R. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+C+J">C. J. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E+S">E. S. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Goto%2C+T">T. Goto</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Holden%2C+B">B. Holden</a>, <a href="/search/astro-ph?searchtype=author&query=Homeier%2C+N">N. Homeier</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">L. Infante</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="astro-ph/0503445v1-abstract-short" style="display: inline;"> We study the dynamical origin of the structures observed in the scattered-light images of the resolved debris disk around HD 141569A. We explore the roles of radiation pressure from the central star, gas drag from the gas disk, and the tidal forces from two nearby stars in creating and maintaining these structures. We use a simple one-dimensional axisymmetric model to show that the presence of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0503445v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0503445v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0503445v1-abstract-full" style="display: none;"> We study the dynamical origin of the structures observed in the scattered-light images of the resolved debris disk around HD 141569A. We explore the roles of radiation pressure from the central star, gas drag from the gas disk, and the tidal forces from two nearby stars in creating and maintaining these structures. We use a simple one-dimensional axisymmetric model to show that the presence of the gas helps confine the dust and that a broad ring of dust is produced if a central hole exists in the disk. This model also suggests that the disk is in a transient, excited dynamical state, as the observed dust creation rate applied over the age of the star is inconsistent with submillimeter mass measurements. We model in two dimensions the effects of a fly-by encounter between the disk and a binary star in a prograde, parabolic, coplanar orbit. We track the spatial distribution of the disk's gas, planetesimals, and dust. We conclude that the surface density distribution reflects the planetesimal distribution for a wide range of parameters. Our most viable model features a disk of initial radius 400 AU, a gas mass of 50 M_earth, and beta = 4 and suggests that the system is being observed within 4000 yr of the fly-by periastron. The model reproduces some features of HD 141569A's disk, such as a broad single ring and large spiral arms, but it does not reproduce the observed multiple spiral rings or disk asymmetries nor the observed clearing in the inner disk. For the latter, we consider the effect of a 5 M_Jup planet in an eccentric orbit on the planetesimal distribution of HD 141569A. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0503445v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0503445v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 627 (2005) 986-1000 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0503365">arXiv:astro-ph/0503365</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0503365">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0503365">ps</a>, <a href="https://arxiv.org/format/astro-ph/0503365">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/430248">10.1086/430248 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evolution in the Cluster Early-type Galaxy Size-Surface Brightness Relation at z =~ 1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holden%2C+B+P">B. P. Holden</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Postman%2C+M">M. Postman</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=IDT%2C+A">ACS IDT</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="astro-ph/0503365v1-abstract-short" style="display: inline;"> We investigate the evolution in the distribution of surface brightness, as a function of size, for elliptical and S0 galaxies in the two clusters RDCS J1252.9-2927, z=1.237 and RX J0152.7-1357, z=0.837. We use multi-color imaging with the Advanced Camera for Surveys on the Hubble Space Telescope to determine these sizes and surface brightnesses. Using three different estimates of the surface bri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0503365v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0503365v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0503365v1-abstract-full" style="display: none;"> We investigate the evolution in the distribution of surface brightness, as a function of size, for elliptical and S0 galaxies in the two clusters RDCS J1252.9-2927, z=1.237 and RX J0152.7-1357, z=0.837. We use multi-color imaging with the Advanced Camera for Surveys on the Hubble Space Telescope to determine these sizes and surface brightnesses. Using three different estimates of the surface brightnesses, we find that we reliably estimate the surface brightness for the galaxies in our sample with a scatter of < 0.2 mag and with systematic shifts of \lesssim 0.05 mag. We construct samples of galaxies with early-type morphologies in both clusters. For each cluster, we use a magnitude limit in a band which closely corresponds to the rest-frame B, to magnitude limit of M_B = -18.8 at z=0, and select only those galaxies within the color-magnitude sequence of the cluster or by using our spectroscopic redshifts. We measure evolution in the rest-frame B surface brightness, and find -1.41 \+/- 0.14 mag from the Coma cluster of galaxies for RDCS J1252.9-2927 and -0.90 \+/- 0.12 mag of evolution for RX J0152.7-1357, or an average evolution of (-1.13 \+/- 0.15) z mag. Our statistical errors are dominated by the observed scatter in the size-surface brightness relation, sigma = 0.42 \+/- 0.05 mag for RX J0152.7-1357 and sigma = 0.76 \+/- 0.10 mag for RDCS J1252.9-2927. We find no statistically significant evolution in this scatter, though an increase in the scatter could be expected. Overall, the pace of luminosity evolution we measure agrees with that of the Fundamental Plane of early-type galaxies, implying that the majority of massive early-type galaxies observed at z =~ 1 formed at high redshifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0503365v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0503365v1-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 March, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2005. </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 in ApJ, 16 pages in emulateapj format with 15 eps figures, 6 in color</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 626 (2005) 809-822 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0412083">arXiv:astro-ph/0412083</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0412083">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0412083">ps</a>, <a href="https://arxiv.org/format/astro-ph/0412083">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/427549">10.1086/427549 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Transformation of Cluster Galaxies at Intermeidate Redshift </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Homeier%2C+N+L">N. L. Homeier</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Postman%2C+M">M. Postman</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L+D">L. D. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Goto%2C+T">T. Goto</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Holden%2C+B">B. Holden</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Jee%2C+M+J">M. J. Jee</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Mei%2C+S">S. Mei</a>, <a href="/search/astro-ph?searchtype=author&query=Menanteau%2C+F">F. Menanteau</a>, <a href="/search/astro-ph?searchtype=author&query=Zirm%2C+A">A. Zirm</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Team%2C+t+A">the ACS Team</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="astro-ph/0412083v1-abstract-short" style="display: inline;"> We combine imaging data from the Advanced Camera for Surveys (ACS) with VLT/FORS optical spectroscopy to study the properties of star-forming galaxies in the z=0.837 cluster CL0152-1357. We have morphological information for 24 star-forming cluster galaxies, which range in morphology from late-type and irregular to compact early-type galaxies. We find that while most star-forming galaxies have… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0412083v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0412083v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0412083v1-abstract-full" style="display: none;"> We combine imaging data from the Advanced Camera for Surveys (ACS) with VLT/FORS optical spectroscopy to study the properties of star-forming galaxies in the z=0.837 cluster CL0152-1357. We have morphological information for 24 star-forming cluster galaxies, which range in morphology from late-type and irregular to compact early-type galaxies. We find that while most star-forming galaxies have $r_{625}-i_{775}$ colors bluer than 1.0, eight are in the red cluster sequence. Among the star-forming cluster population we find five compact early-type galaxies which have properties consistent with their identification as progenitors of dwarf elliptical galaxies. The spatial distribution of the star-forming cluster members is nonuniform. We find none within $R\sim 500$ Mpc of the cluster center, which is highly suggestive of an intracluster medium interaction. We derive star formation rates from [OII] $位位3727$ line fluxes, and use these to compare the global star formation rate of CL0152-1357 to other clusters at low and intermediate redshifts. We find a tentative correlation between integrated star formation rates and $T_{X}$, in the sense that hotter clusters have lower integrated star formation rates. Additional data from clusters with low X-ray temperatures is needed to confirm this trend. We do not find a significant correlation with redshift, suggesting that evolution is either weak or absent between z=0.2-0.8. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0412083v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0412083v1-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, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2004. </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">ApJ accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 621 (2005) 651-662 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0411516">arXiv:astro-ph/0411516</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0411516">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0411516">ps</a>, <a href="https://arxiv.org/format/astro-ph/0411516">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/427492">10.1086/427492 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Luminosity Functions of the Galaxy Cluster MS1054-0321 at z=0.83 based on ACS Photometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Goto%2C+T">Tomotsugu Goto</a>, <a href="/search/astro-ph?searchtype=author&query=Postman%2C+M">Marc Postman</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">Nicholas J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Tran%2C+K">K. Tran</a>, <a href="/search/astro-ph?searchtype=author&query=Magee%2C+D">D. Magee</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Homeier%2C+N+L">N. L. Homeier</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Menanteau%2C+F">F. Menanteau</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L+D">L. D. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R+A">R. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+C+J">C. J. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E+S">E. S. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</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="astro-ph/0411516v4-abstract-short" style="display: inline;"> We present new measurements of the galaxy luminosity function (LF) and its dependence on local galaxy density, color, morphology, and clustocentric radius for the massive z=0.83 cluster MS1054-0321. Our analyses are based on imaging performed with the ACS onboard the HST in the F606W, F775W and F850LP passbands and extensive spectroscopic data obtained with the Keck LRIS. Our main results are ba… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0411516v4-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0411516v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0411516v4-abstract-full" style="display: none;"> We present new measurements of the galaxy luminosity function (LF) and its dependence on local galaxy density, color, morphology, and clustocentric radius for the massive z=0.83 cluster MS1054-0321. Our analyses are based on imaging performed with the ACS onboard the HST in the F606W, F775W and F850LP passbands and extensive spectroscopic data obtained with the Keck LRIS. Our main results are based on a spectroscopically selected sample of 143 cluster members with morphological classifications derived from the ACS observations. Our three primary findings are (1) the faint-end slope of the LF is steepest in the bluest filter, (2) the LF in the inner part of the cluster (or highest density regions) has a flatter faint-end slope, and (3) the fraction of early-type galaxies is higher at the bright end of the LF, and gradually decreases toward fainter magnitudes. These characteristics are consistent with those in local galaxy clusters, indicating that, at least in massive clusters, the common characteristics of cluster LFs are established at z=0.83. We also find a 2sigma deficit of intrinsically faint, red galaxies (i-z>0.5, Mi>-19) in this cluster. This trend may suggest that faint, red galaxies (which are common in z<0.1 rich clusters) have not yet been created in this cluster at z=0.83. The giant-to-dwarf ratio in MS1054-0321 starts to increase inwards of the virial radius or when Sigma>30 Mpc^-2, coinciding with the environment where the galaxy star formation rate and the morphology-density relation start to appear. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0411516v4-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0411516v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2004; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 November, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2004. </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">ApJ in press, references updated</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 621 (2005) 188-200 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0411148">arXiv:astro-ph/0411148</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0411148">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0411148">ps</a>, <a href="https://arxiv.org/format/astro-ph/0411148">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/425628">10.1086/425628 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dust and Ionized Gas in Nine Nearby Early-Type Galaxies Imaged with the HST Advanced Camera for Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L+D">L. D. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Tran%2C+H+D">H. D. Tran</a>, <a href="/search/astro-ph?searchtype=author&query=Menanteau%2C+F">F. Menanteau</a>, <a href="/search/astro-ph?searchtype=author&query=Tsvetanov%2C+Z+I">Z. I. Tsvetanov</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</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="astro-ph/0411148v1-abstract-short" style="display: inline;"> We present $V$ and $I$ continuum images and H$伪$+[N II] maps of nine early-type galaxies observed with the Wide Field Channel of the Advanced Camera for Surveys on the Hubble Space Telescope. Dust and ionized gas are detected in all galaxies. The optical nebulae are primarily concentrated on the nuclei and extend out to radii of a few hundred parsecs, in compact clumps, filaments, or disks. Two… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0411148v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0411148v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0411148v1-abstract-full" style="display: none;"> We present $V$ and $I$ continuum images and H$伪$+[N II] maps of nine early-type galaxies observed with the Wide Field Channel of the Advanced Camera for Surveys on the Hubble Space Telescope. Dust and ionized gas are detected in all galaxies. The optical nebulae are primarily concentrated on the nuclei and extend out to radii of a few hundred parsecs, in compact clumps, filaments, or disks. Two galaxies, NGC 6166 and NGC 6338, also possess diffuse, ionized filaments on kiloparsec scales. The ionized gas is entirely contained within the nuclear disks of ESO 208-G021, NGC 3078, and NGC 7720. In the radio-loud galaxy NGC 6166, emission-line filaments are detected along the radio lobes, possibly as a result of shock ionization. A wide range of ionized gas masses, $M_g\approx7\times10^2-3\times10^6$ $M_\odot$, are calculated from the observed fluxes. Even in this small sample, the orientation of the ionized material correlates well with the major or minor axis of the galaxies, consistent with an external origin for the dust and gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0411148v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0411148v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 November, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2004. </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, to appear Dec 4, 2004. 14 pages, 4 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/astro-ph/0411125">arXiv:astro-ph/0411125</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0411125">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0411125">ps</a>, <a href="https://arxiv.org/format/astro-ph/0411125">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/427232">10.1086/427232 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Nature of Blue Cores in Spheroids: a Possible Connection with AGN and Star Formation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Menanteau%2C+F">Felipe Menanteau</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">Paolo Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">Brenda Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">Holland C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">Leopoldo Infante</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">Narciso Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Galaz%2C+G">Gaspar Galaz</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Daniel Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">Garth D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">George F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">Marc Clampin</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="astro-ph/0411125v1-abstract-short" style="display: inline;"> We investigate the physical nature of blue cores in early-type galaxies through the first multi-wavelength analysis of a serendipitously discovered field blue-nucleated spheroid in the background of the deep ACS/WFC griz multicolor observations of the cluster Abell 1689. The resolved g-r, r-i and i-z color maps reveal a prominent blue core identifying this galaxy as a ``typical'' case study, exh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0411125v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0411125v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0411125v1-abstract-full" style="display: none;"> We investigate the physical nature of blue cores in early-type galaxies through the first multi-wavelength analysis of a serendipitously discovered field blue-nucleated spheroid in the background of the deep ACS/WFC griz multicolor observations of the cluster Abell 1689. The resolved g-r, r-i and i-z color maps reveal a prominent blue core identifying this galaxy as a ``typical'' case study, exhibiting variations of 0.5-1.0 mag in color between the center and the outer regions, opposite to the expectations of reddened metallicity induced gradients in passively evolved ellipticals. From a Magellan-Clay spectrum we secure the galaxy redshift at $z=0.624$. We find a strong X-ray source coincident with the spheroid galaxy. Spectral features and a high X-ray luminosity indicate the presence of an AGN in the galaxy. However, a comparison of the X-ray luminosity to a sample derived from the Chandra Deep Field South displays Lx to be comparable to Type I/QSO galaxies while the optical flux is consistent with a normal star-forming galaxy. We conclude that the galaxy's non-thermal component dominates at high-energy wavelengths while we associate the spheroid blue light with the stellar spectrum of normal star-forming galaxies. We argue about a probable association between the presence of blue cores in spheroids and AGN activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0411125v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0411125v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2004. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal. 6 pages, 3 figures. Full resolution images available at http://acs.pha.jhu.edu/~felipe/e-prints</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 620 (2005) 697-702 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0407644">arXiv:astro-ph/0407644</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0407644">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0407644">ps</a>, <a href="https://arxiv.org/format/astro-ph/0407644">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/424857">10.1086/424857 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Luminosity Function of Early-Type Galaxies at z~0.75 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R">R. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Menanteau%2C+F">F. Menanteau</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Goto%2C+T">T. Goto</a>, <a href="/search/astro-ph?searchtype=author&query=Holden%2C+B">B. Holden</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Overzier%2C+R">R. Overzier</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Homeier%2C+N">N. Homeier</a>, <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R+A">R. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+C+J">C. J. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E+S">E. S. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">L. Infante</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="astro-ph/0407644v1-abstract-short" style="display: inline;"> We measure the luminosity function of morphologically selected E/S0 galaxies from $z=0.5$ to $z=1.0$ using deep high resolution Advanced Camera for Surveys imaging data. Our analysis covers an area of $48\Box\arcmin$ (8$\times$ the area of the HDF-N) and extends 2 magnitudes deeper ($I\sim24$ mag) than was possible in the Deep Groth Strip Survey (DGSS). At $0.5<z<0.75$, we find… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0407644v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0407644v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0407644v1-abstract-full" style="display: none;"> We measure the luminosity function of morphologically selected E/S0 galaxies from $z=0.5$ to $z=1.0$ using deep high resolution Advanced Camera for Surveys imaging data. Our analysis covers an area of $48\Box\arcmin$ (8$\times$ the area of the HDF-N) and extends 2 magnitudes deeper ($I\sim24$ mag) than was possible in the Deep Groth Strip Survey (DGSS). At $0.5<z<0.75$, we find $M_B^*-5\log h_{0.7}=-21.1\pm0.3$ and $伪=-0.53\pm0.2$, and at $0.75<z<1.0$, we find $M_B^*-5\log h_{0.7}=-21.4\pm0.2$. These luminosity functions are similar in both shape and number density to the luminosity function using morphological selection (e.g., DGSS), but are much steeper than the luminosity functions of samples selected using morphological proxies like the color or spectral energy distribution (e.g., CFRS, CADIS, or COMBO-17). The difference is due to the `blue', $(U-V)_0<1.7$, E/S0 galaxies, which make up to $\sim30%$ of the sample at all magnitudes and an increasing proportion of faint galaxies. We thereby demonstrate the need for {\it both morphological and structural information} to constrain the evolution of galaxies. We find that the `blue' E/S0 galaxies have the same average sizes and Sersic parameters as the `red', $(U-V)_0>1.7$, E/S0 galaxies at brighter luminosities ($M_B<-20.1$), but are increasingly different at fainter magnitudes where `blue' galaxies are both smaller and have lower Sersic parameters. Fits of the colors to stellar population models suggest that most E/S0 galaxies have short star-formation time scales ($蟿<1$ Gyr), and that galaxies have formed at an increasing rate from $z\sim8$ until $z\sim2$ after which there has been a gradual decline. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0407644v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0407644v1-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 July, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2004. </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, 21 figures, accepted in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0406613">arXiv:astro-ph/0406613</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0406613">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0406613">ps</a>, <a href="https://arxiv.org/format/astro-ph/0406613">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/423701">10.1086/423701 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ultra Compact Dwarf galaxies in Abell 1689: a photometric study with the ACS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">S. Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">L. Infante</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">D. Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Zekser%2C+K">K. Zekser</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H">H. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R+A">R. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+C+J">C. J. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E+S">E. S. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Goto%2C+T">T. Goto</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Holden%2C+B">B. Holden</a>, <a href="/search/astro-ph?searchtype=author&query=Homeier%2C+N">N. Homeier</a> , et al. (15 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="astro-ph/0406613v1-abstract-short" style="display: inline;"> The properties of Ultra Compact Dwarf (UCD) galaxy candidates in Abell 1689 (z=0.183) are investigated, based on deep high resolution ACS images. A UCD candidate has to be unresolved, have i<28 (M_V<-11.5) mag and satisfy color limits derived from Bayesian photometric redshifts. We find 160 UCD candidates with 22<i<28 mag. It is estimated that about 100 of these are cluster members, based on the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0406613v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0406613v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0406613v1-abstract-full" style="display: none;"> The properties of Ultra Compact Dwarf (UCD) galaxy candidates in Abell 1689 (z=0.183) are investigated, based on deep high resolution ACS images. A UCD candidate has to be unresolved, have i<28 (M_V<-11.5) mag and satisfy color limits derived from Bayesian photometric redshifts. We find 160 UCD candidates with 22<i<28 mag. It is estimated that about 100 of these are cluster members, based on their spatial distribution and photometric redshifts. For i>26.8 mag, the radial and luminosity distribution of the UCD candidates can be explained well by Abell 1689's globular cluster (GC) system. For i<26.8 mag, there is an overpopulation of 15 +/- 5 UCD candidates with respect to the GC luminosity function. For i<26 mag, the radial distribution of UCD candidates is more consistent with the dwarf galaxy population than with the GC system of Abell 1689. The UCD candidates follow a color-magnitude trend with a slope similar to that of Abell 1689's genuine dwarf galaxy population, but shifted fainter by about 2-3 mag. Two of the three brightest UCD candidates (M_V ~ -17 mag) are slightly resolved. At the distance of Abell 1689, these two objects would have King-profile core radii of ~35 pc and r_eff ~300 pc, implying luminosities and sizes 2-3 times those of M32's bulge. Additional photometric redshifts obtained with late type stellar and elliptical galaxy templates support the assignment of these two resolved sources to Abell 1689. Our findings imply that in Abell 1689 there are at least 10 UCDs with M_V<-12.7 mag. Compared to the UCDs in the Fornax cluster they are brighter, larger and have colors closer to normal dwarf galaxies. This suggests that they may be in an intermediate stage of the stripping process. Spectroscopy is needed to definitely confirm the existence of UCDs in Abell 1689. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0406613v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0406613v1-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 June, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2004. </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">29 pages, 10 figures, accepted for publication in the October 2004 issue of the Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0405326">arXiv:astro-ph/0405326</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0405326">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0405326">ps</a>, <a href="https://arxiv.org/format/astro-ph/0405326">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/422568">10.1086/422568 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Internal Color Properties of Resolved Spheroids in the Deep HST/ACS field of UGC 10214 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Menanteau%2C+F">F. Menanteau</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Sirianni%2C+M">M. Sirianni</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G+R">G. R. Meurer</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Postman%2C+M">M. Postman</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R+A">R. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+C+J">C. J. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E+S">E. S. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">L. Infante</a>, <a href="/search/astro-ph?searchtype=author&query=Kimble%2C+R+A">R. A. Kimble</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="astro-ph/0405326v2-abstract-short" style="display: inline;"> (Abridged) We study the internal color properties of a morphologically selected sample of spheroidal galaxies taken from HST/ACS ERO program of UGC 10214 (``The Tadpole''). By taking advantage of the unprecedented high resolution of the ACS in this very deep dataset we are able to characterize spheroids at sub-arcseconds scales. Using the V_606W and I_814W bands, we construct V-I color maps and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0405326v2-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0405326v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0405326v2-abstract-full" style="display: none;"> (Abridged) We study the internal color properties of a morphologically selected sample of spheroidal galaxies taken from HST/ACS ERO program of UGC 10214 (``The Tadpole''). By taking advantage of the unprecedented high resolution of the ACS in this very deep dataset we are able to characterize spheroids at sub-arcseconds scales. Using the V_606W and I_814W bands, we construct V-I color maps and extract color gradients for a sample of spheroids at I_814W < 24 mag. We investigate the existence of a population of morphologically classified spheroids which show extreme variation in their internal color properties similar to the ones reported in the HDFs. These are displayed as blue cores and inverse color gradients with respect to those accounted from metallicity variations. Following the same analysis we find a similar fraction of early-type systems (~30%-40%) that show non-homologous internal colors, suggestive of recent star formation activity. We present two statistics to quantify the internal color variation in galaxies and for tracing blue cores, from which we estimate the fraction of non-homogeneous to homogeneous internal colors as a function of redshift up to z<1.2. We find that it can be described as about constant as a function of redshift, with a small increase with redshift for the fraction of spheroids that present strong color dispersions. The implications of a constant fraction at all redshifts suggests the existence of a relatively permanent population of evolving spheroids up to z~1. We discuss the implications of this in the context of spheroidal formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0405326v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0405326v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 May, 2004; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 May, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2004. </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">Fixed URL for high resolution version. 13 Pages, 10 Figures. Accepted for Publication in ApJ. Sep 1st issue. Higher resolution version and complete table3B at http://acs.pha.jhu.edu/~felipe/e-prints/Tadpole</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 612 (2004) 202-214 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0311323">arXiv:astro-ph/0311323</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0311323">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0311323">ps</a>, <a href="https://arxiv.org/format/astro-ph/0311323">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/381317">10.1086/381317 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of Globular Clusters in the Proto-Spiral NGC2915: Implications for Hierarchical Galaxy Evolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G+R">G. R. Meurer</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Sirianni%2C+M">M. Sirianni</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Menanteau%2C+F">F. Menanteau</a>, <a href="/search/astro-ph?searchtype=author&query=Tran%2C+H+D">H. D. Tran</a>, <a href="/search/astro-ph?searchtype=author&query=Kimble%2C+R+A">R. A. Kimble</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R+A">R. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+C+J">C. J. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E+S">E. S. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">L. Infante</a>, <a href="/search/astro-ph?searchtype=author&query=Krist%2C+J+E">J. E. Krist</a>, <a href="/search/astro-ph?searchtype=author&query=Lesser%2C+M+P">M. P. Lesser</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="astro-ph/0311323v1-abstract-short" style="display: inline;"> We have discovered three globular clusters beyond the Holmberg radius in Hubble Space Telescope Advanced Camera for Surveys images of the gas-rich dark matter dominated blue compact dwarf galaxy NGC2915. The clusters, all of which start to resolve into stars, have M_{V606} = -8.9 to -9.8 mag, significantly brighter than the peak of the luminosity function of Milky Way globular clusters. Their co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0311323v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0311323v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0311323v1-abstract-full" style="display: none;"> We have discovered three globular clusters beyond the Holmberg radius in Hubble Space Telescope Advanced Camera for Surveys images of the gas-rich dark matter dominated blue compact dwarf galaxy NGC2915. The clusters, all of which start to resolve into stars, have M_{V606} = -8.9 to -9.8 mag, significantly brighter than the peak of the luminosity function of Milky Way globular clusters. Their colors suggest a metallicity [Fe/H] ~ -1.9 dex, typical of metal-poor Galactic globular clusters. The specific frequency of clusters is at a minimum normal, compared to spiral galaxies. However, since only a small portion of the system has been surveyed it is more likely that the luminosity and mass normalized cluster content is higher, like that seen in elliptical galaxies and galaxy clusters. This suggests that NGC2915 resembles a key phase in the early hierarchical assembly of galaxies - the epoch when much of the old stellar population has formed, but little of the stellar disk. Depending on the subsequent interaction history, such systems could go on to build-up larger elliptical galaxies, evolve into normal spirals, or in rare circumstances remain suspended in their development to become systems like NGC2915. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0311323v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0311323v1-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, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2003. </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">ApJ Letters accepted; 6 pages, 2 figures, 3 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 599 (2003) L83-L86 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0309077">arXiv:astro-ph/0309077</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0309077">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0309077">ps</a>, <a href="https://arxiv.org/format/astro-ph/0309077">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/380120">10.1086/380120 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Faint Galaxies in deep ACS observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H">H. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R">R. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Menanteau%2C+F">F. Menanteau</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J">J. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G">G. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G">G. Meurer</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G">G. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Magee%2C+D">D. Magee</a>, <a href="/search/astro-ph?searchtype=author&query=Sirianni%2C+M">M. Sirianni</a>, <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R+A">R. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+C+J">C. J. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E+S">E. S. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">L. Infante</a>, <a href="/search/astro-ph?searchtype=author&query=Kimble%2C+R+A">R. A. Kimble</a>, <a href="/search/astro-ph?searchtype=author&query=Krist%2C+J+E">J. E. Krist</a> , et al. (11 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="astro-ph/0309077v1-abstract-short" style="display: inline;"> We present the analysis of the faint galaxy population in the Advanced Camera for Surveys (ACS) Early Release Observation fields VV 29 (UGC 10214) and NGC 4676. Here we attempt to thoroughly consider all aspects relevant for faint galaxy counting and photometry, developing methods which are based on public software and that are easily reproducible by other astronomers. Using simulations we deter… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0309077v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0309077v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0309077v1-abstract-full" style="display: none;"> We present the analysis of the faint galaxy population in the Advanced Camera for Surveys (ACS) Early Release Observation fields VV 29 (UGC 10214) and NGC 4676. Here we attempt to thoroughly consider all aspects relevant for faint galaxy counting and photometry, developing methods which are based on public software and that are easily reproducible by other astronomers. Using simulations we determine the best SExtractor parameters for the detection of faint galaxies in deep HST observations, paying special attention to the issue of deblending, which significantly affects the normalization and shape of the number count distribution. We confirm, as claimed by Bernstein, Freedman and Madore (2002), that Kron-like magnitudes, such as the ones generated by SExtractor, can miss more than half of the light of faint galaxies, what dramatically affects the slope of the number counts. We present catalogs for the VV 29 and NGC 4676 fields with photometry in the g,V and I bands. We also show that combining the bayesian software BPZ with superb ACS data and new spectral templates enables us to estimate reliable photometric redshifts for a significant fraction of galaxies with as few as three filters. After correcting for selection effects, we measure slopes of 0.32+- 0.01 for 22 < g < 28, 0.34+-0.01 for 22< V <27.5 and 0.33+-0.01 for 22 < I < 27. The counts do not flatten (except perhaps in the g-band), up to the depth of our observations. We find that the faint counts m_{AB}> 25.5 can be well approximated in all our filters by a passive luminosity evolution model based on the COMBO-17 luminosity function (伪=-1.5), with a strong merging rate following the prescription of Glazebrook et al. (1994), 蠁^*\propto (1+Qz), with Q=4. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0309077v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0309077v1-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 September, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2003. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 20 figures, to appear in ApJS. Several figures heavily degraded to fit astro-ph size limit. Please download full resolution version from http://acs.pha.jhu.edu/~txitxo/FaintGalaxies.ps.gz</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0309036">arXiv:astro-ph/0309036</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0309036">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0309036">ps</a>, <a href="https://arxiv.org/format/astro-ph/0309036">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/379234">10.1086/379234 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Advanced Camera for Surveys Photometry of the Cluster RDCS1252.9-2927: The Color-Magnitude Relation at z=1.24 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Postman%2C+M">M. Postman</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Holden%2C+B+P">B. P. Holden</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">L. Infante</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Miley%2C+G+K">G. K. Miley</a>, <a href="/search/astro-ph?searchtype=author&query=Menanteau%2C+F">F. Menanteau</a>, <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G+R">G. R. Meurer</a>, <a href="/search/astro-ph?searchtype=author&query=Sirianni%2C+M">M. Sirianni</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+R+L">R. L. White</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="astro-ph/0309036v1-abstract-short" style="display: inline;"> We investigate the color-magnitude (CM) relation of galaxies in the distant X-ray selected cluster RDCS1252.9-2927 at z=1.24 using images obtained with the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope in the F775W and F850LP bandpasses. We select galaxies based on morphological classifications extending about 3.5 mag down the galaxy luminosity function, augmented by spectrosco… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0309036v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0309036v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0309036v1-abstract-full" style="display: none;"> We investigate the color-magnitude (CM) relation of galaxies in the distant X-ray selected cluster RDCS1252.9-2927 at z=1.24 using images obtained with the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope in the F775W and F850LP bandpasses. We select galaxies based on morphological classifications extending about 3.5 mag down the galaxy luminosity function, augmented by spectroscopic membership information. At the core of the cluster is an extensive early-type galaxy population surrounding a central pair of galaxies that show signs of dynamical interaction. The early-type population defines a tight sequence in the CM diagram, with an intrinsic scatter in observed (i-z) of $0.029\pm0.007$ mag based on 52 galaxies, or $0.024\pm0.008$ mag for $\sim30$ ellipticals. Simulations using the latest stellar population models indicate an age scatter for the ellipticals of about 34%, with a mean age $\taul\gta2.6$ Gyr (corresponding to $z_L\gta2.7$), and the last star formation occurring at $z_{end}\gta1.5$. Transforming to rest-frame $(U-B)$, we conclude that the slope and scatter in the CM relation for morphologically selected early-type galaxies show little or no evidence for evolution out to $z\approx1.2$. Thus, elliptical galaxies were already well established in X-ray luminous clusters when the universe was a third of its present age. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0309036v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0309036v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 September, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2003. </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 emulateapj pages with 4 figures, including a bonus figure not seen elsewhere. Accepted for publication in ApJ Letters. A version with a higher resolution fig 1 can be found at http://acs.pha.jhu.edu/~jpb/z1clusters/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.596:L143-L146,2003 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0308201">arXiv:astro-ph/0308201</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0308201">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0308201">ps</a>, <a href="https://arxiv.org/format/astro-ph/0308201">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1051/0004-6361:20031343">10.1051/0004-6361:20031343 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chandra Discovery of an X-ray Jet and Lobes in 3C 15 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kataoka%2C+J">J. Kataoka</a>, <a href="/search/astro-ph?searchtype=author&query=Leahy%2C+J+P">J. P. Leahy</a>, <a href="/search/astro-ph?searchtype=author&query=Edwards%2C+P+G">P. G. Edwards</a>, <a href="/search/astro-ph?searchtype=author&query=Kino%2C+M">M. Kino</a>, <a href="/search/astro-ph?searchtype=author&query=Takahara%2C+F">F. Takahara</a>, <a href="/search/astro-ph?searchtype=author&query=Serino%2C+Y">Y. Serino</a>, <a href="/search/astro-ph?searchtype=author&query=Kawai%2C+N">N. Kawai</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</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="astro-ph/0308201v1-abstract-short" style="display: inline;"> We report the Chandra detection of an X-ray jet in 3C 15. The peak of the X-ray emission in the jet is 4.1'' (a projected distance of 5.1 kpc) from the nucleus, and coincident with a component previously identified in the radio and optical jets. We examine four models for the X-ray jet emission: (I) weak synchrotron cooling in equip., (II) moderate synchrotron cooling in equip., (III) weak synch… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0308201v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0308201v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0308201v1-abstract-full" style="display: none;"> We report the Chandra detection of an X-ray jet in 3C 15. The peak of the X-ray emission in the jet is 4.1'' (a projected distance of 5.1 kpc) from the nucleus, and coincident with a component previously identified in the radio and optical jets. We examine four models for the X-ray jet emission: (I) weak synchrotron cooling in equip., (II) moderate synchrotron cooling in equip., (III) weak synchrotron plus SSC cooling, and (IV) moderate synchrotron plus SSC cooling. We argue that case (II) can most reasonably explain the overall emission from knot C. Case (III) is also possible, but requires a large departure from equipartition and for the jet power to be comparable to that of the brightest quasars. Diffuse X-ray emission has also been detected, distributed widely over the full extent (63kpc x 25kpc) of the radio lobes. We compare the total energy contained in the lobes with the jet power estimated from knot C, and discuss the energetic link between the jet and the lobes. We argue that the fueling time (t_fuel) and the source age (t_src) are comparable for case (II), whereas t_fuel << t_src is likely for case (III). The latter may imply that the jet has a very small filling factor, ~10^{-3}. We consider the pressure balance between the thermal galaxy halo and non-thermal relativistic electrons in the radio lobes. Finally, we show that the X-ray emission from the nucleus is not adequately fitted by a simple absorbed power-law model, but needs an additional power-law with heavy absorption intrinsic to the source. Such a high column density is consistent with the presence of a dense, dusty torus which obscures the quasar nucleus. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0308201v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0308201v1-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 August, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2003. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 8 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.Astrophys.410:833-846,2003 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0306215">arXiv:astro-ph/0306215</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0306215">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0306215">ps</a>, <a href="https://arxiv.org/format/astro-ph/0306215">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/377477">10.1086/377477 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Star Formation at z~6: i-dropouts in the ACS GTO fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T">T. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Magee%2C+D">D. Magee</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G+R">G. R. Meurer</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R+A">R. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+C+J">C. J. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E+S">E. S. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">L. Infante</a>, <a href="/search/astro-ph?searchtype=author&query=Kimble%2C+R+A">R. A. Kimble</a>, <a href="/search/astro-ph?searchtype=author&query=Krist%2C+J+E">J. E. Krist</a> , et al. (11 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="astro-ph/0306215v1-abstract-short" style="display: inline;"> Using an i-z dropout criterion, we determine the space density of z~6 galaxies from two deep ACS GTO fields with deep optical-IR imaging. A total of 23 objects are found over 46 arcmin^2, or ~0.5 objects/arcmin^2 down to z~27.3 (6 sigma; all AB mag) (including one probable z~6 AGN). Combining deep ISAAC data for our RDCS1252-2927 field (J~25.7 and Ks~25.0 (5 sigma)) and NICMOS data for the HDF N… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0306215v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0306215v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0306215v1-abstract-full" style="display: none;"> Using an i-z dropout criterion, we determine the space density of z~6 galaxies from two deep ACS GTO fields with deep optical-IR imaging. A total of 23 objects are found over 46 arcmin^2, or ~0.5 objects/arcmin^2 down to z~27.3 (6 sigma; all AB mag) (including one probable z~6 AGN). Combining deep ISAAC data for our RDCS1252-2927 field (J~25.7 and Ks~25.0 (5 sigma)) and NICMOS data for the HDF North (JH~27.3 (5 sigma)), we verify that these dropouts have flat spectral slopes. i-dropouts in our sample range in luminosity from ~1.5 L* (z~25.6) to ~0.3 L* (z~27.3) with the exception of one very bright candidate at z~24.2. The half-light radii vary from 0.09" to 0.29", or 0.5 kpc to 1.7 kpc. We derive the z~6 rest-frame UV luminosity density using three different procedures, each utilizing simulations based on a CDF South V dropout sample. First, we compare our findings with a no-evolution projection of this V-dropout sample. We find 23+/-25% more i-dropouts than we predict. Adopting previous results to z~5, this works out to a 20+/-29% drop in the luminosity density from z~3 to z~6. Second, we use these same V-dropout simulations to derive a selection function for our i-dropout sample and compute the UV-luminosity density (7.2+/-2.5 x 10^25 ergs/s/Hz/Mpc^3 down to z~27). We find a 39+/-21% drop over the same redshift range. This is our preferred value and suggests a star formation rate of 0.0090+/-0.0031 M_sol/yr/Mpc^3 to z~27, or ~0.036+/- 0.012 M_sol/yr/Mpc^3 extrapolating the LF to the faint limit. Third, we follow a very similar procedure, but assume no incompleteness, finding a luminosity density which is ~2-3X lower. This final estimate constitutes a lower limit. All three estimates are within the canonical range of luminosity densities necessary for reionization of the universe at this epoch. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0306215v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0306215v1-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 June, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2003. </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">36 pages, 13 figures, 2 tables, accepted for publication in ApJ, postscript version with high-resolution figures can be downloaded at http://www.ucolick.org/~bouwens/idropout.ps</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.595:589-602,2003 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0303605">arXiv:astro-ph/0303605</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0303605">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0303605">ps</a>, <a href="https://arxiv.org/format/astro-ph/0303605">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/375460">10.1086/375460 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HST/ACS Coronagraphic Imaging of the Circumstellar Disk around HD1415659A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Krist%2C+J+E">J. E. Krist</a>, <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R+A">R. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+C+J">C. J. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E+S">E. S. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">L. Infante</a>, <a href="/search/astro-ph?searchtype=author&query=Kimble%2C+R+A">R. A. Kimble</a>, <a href="/search/astro-ph?searchtype=author&query=Lesser%2C+M+P">M. P. Lesser</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Menanteau%2C+F">F. Menanteau</a>, <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G+R">G. R. Meurer</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0303605v1-abstract-short" style="display: inline;"> Multicolor coronagraphic images of the circumstellar disk around HD141569A have been obtained with the Hubble Space Telescope (HST) Advanced Camera for Surveys. B, V, and I images show that the disk's previously-described multiple-ring structure is actually a continuous distribution of dust with a tightly-wound spiral structure. Two, more open spiral arms extend from the disk, one of which appea… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0303605v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0303605v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0303605v1-abstract-full" style="display: none;"> Multicolor coronagraphic images of the circumstellar disk around HD141569A have been obtained with the Hubble Space Telescope (HST) Advanced Camera for Surveys. B, V, and I images show that the disk's previously-described multiple-ring structure is actually a continuous distribution of dust with a tightly-wound spiral structure. Two, more open spiral arms extend from the disk, one of which appears to reach the nearby binary star HD141569BC. Diffuse dust is seen up to 1200AU from HD141569A. Although planets may exist in the inner region of the disk, tidal interaction with HD141569BC seems more likely to be the cause of these phenomena. The disk appears redder than the star (B-V = 0.21 and V-I = 0.25), and its color is spatially uniform. A scattering asymmetry factor of g = 0.25-0.35 is derived. The azimuthal density distribution is asymmetric, varying by a factor of ~3 at some radii. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0303605v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0303605v1-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, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2003. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 9 figures, accepted in the Astronomical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.J. 126 (2003) 385 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0302402">arXiv:astro-ph/0302402</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0302402">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0302402">ps</a>, <a href="https://arxiv.org/format/astro-ph/0302402">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/374797">10.1086/374797 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of Two Distant Type Ia Supernovae in the Hubble Deep Field North with the Advanced Camera for Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Tsvetanov%2C+Z+I">Zlatan I. Tsvetanov</a>, <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">Holland C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">Garth D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Magee%2C+D">Daniel Magee</a>, <a href="/search/astro-ph?searchtype=author&query=Tonry%2C+J+L">John L. Tonry</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G+R">G. R. Meurer</a>, <a href="/search/astro-ph?searchtype=author&query=Sirianni%2C+M">M. Sirianni</a>, <a href="/search/astro-ph?searchtype=author&query=Ardila%2C+D+R">D. R. Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R">R. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T">T. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N">N. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Kimble%2C+R">R. Kimble</a>, <a href="/search/astro-ph?searchtype=author&query=Krist%2C+J">J. Krist</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Menanteau%2C+F">F. Menanteau</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="astro-ph/0302402v1-abstract-short" style="display: inline;"> We present observations of the first two supernovae discovered with the recently installed Advanced Camera for Surveys (ACS) on the Hubble Space Telescope. The supernovae were found in Wide Field Camera images of the Hubble Deep Field North taken with the F775W, F850LP, and G800L optical elements as part of the ACS guaranteed time observation program. Spectra extracted from the ACS G800L grism e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0302402v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0302402v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0302402v1-abstract-full" style="display: none;"> We present observations of the first two supernovae discovered with the recently installed Advanced Camera for Surveys (ACS) on the Hubble Space Telescope. The supernovae were found in Wide Field Camera images of the Hubble Deep Field North taken with the F775W, F850LP, and G800L optical elements as part of the ACS guaranteed time observation program. Spectra extracted from the ACS G800L grism exposures confirm that the objects are Type Ia supernovae (SNe Ia) at redshifts z=0.47 and z=0.95. Follow-up HST observations have been conducted with ACS in F775W and F850LP and with NICMOS in the near-infrared F110W bandpass, yielding a total of 9 flux measurements in the 3 bandpasses over a period of 50 days in the observed frame. We discuss many of the important issues in doing accurate photometry with the ACS. We analyze the multi-band light curves using two different fitting methods to calibrate the supernovae luminosities and place them on the SNe Ia Hubble diagram. The resulting distances are consistent with the redshift-distance relation of the accelerating universe model, although evolving intergalactic grey dust remains as a less likely possibility. The relative ease with which these SNe Ia were found, confirmed, and monitored demonstrates the potential ACS holds for revolutionizing the field of high-redshift SNe Ia, and therefore of testing the accelerating universe cosmology and constraining the "epoch of deceleration". <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0302402v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0302402v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 February, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2003. </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, 8 embedded figures. Accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 589 (2003) 693-703 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0212208">arXiv:astro-ph/0212208</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0212208">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0212208">ps</a>, <a href="https://arxiv.org/format/astro-ph/0212208">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> Calibration of Geometric Distortion in the ACS Detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G+R">G. R. Meurer</a>, <a href="/search/astro-ph?searchtype=author&query=Lindler%2C+D">D. Lindler</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cox%2C+C">C. Cox</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Tran%2C+H+D">H. D. Tran</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R+J">R. J. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G+F">G. F. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Sirianni%2C+M">M. Sirianni</a>, <a href="/search/astro-ph?searchtype=author&query=de+Marchi%2C+G">G. de Marchi</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="astro-ph/0212208v1-abstract-short" style="display: inline;"> The off-axis location of the Advanced Camera for Surveys (ACS) is the chief (but not sole) cause of strong geometric distortion in all detectors: the Wide Field Camera (WFC), High Resolution Camera (HRC), and Solar Blind Camera (SBC). Dithered observations of rich star cluster fields are used to calibrate the distortion. We describe the observations obtained, the algorithms used to perform the c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0212208v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0212208v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0212208v1-abstract-full" style="display: none;"> The off-axis location of the Advanced Camera for Surveys (ACS) is the chief (but not sole) cause of strong geometric distortion in all detectors: the Wide Field Camera (WFC), High Resolution Camera (HRC), and Solar Blind Camera (SBC). Dithered observations of rich star cluster fields are used to calibrate the distortion. We describe the observations obtained, the algorithms used to perform the calibrations and the accuracy achieved. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0212208v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0212208v1-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 December, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2002. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">to appear in "Proceedings of the 2002 HST Calibration Workshop", S. Arribas, A. Koekemoer, and B. Whitmore, eds.; 4 pages, 2 figures each containing two panels</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0211371">arXiv:astro-ph/0211371</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0211371">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0211371">ps</a>, <a href="https://arxiv.org/format/astro-ph/0211371">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/346125">10.1086/346125 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Advanced Camera for Surveys Observations of Young Star Clusters in the Interacting Galaxy UGC 10214 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tran%2C+H+D">Hien D. Tran</a>, <a href="/search/astro-ph?searchtype=author&query=Sirianni%2C+M">M. Sirianni</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+H+C">H. C. Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Illingworth%2C+G+D">G. D. Illingworth</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+G">G. Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+R+H">R. H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+R+L">R. L. White</a>, <a href="/search/astro-ph?searchtype=author&query=Bartko%2C+F">F. Bartko</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwens%2C+R">R. Bouwens</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">T. J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R">R. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+C">C. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E">E. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N">N. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">M. Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Golimowski%2C+D+A">D. A. Golimowski</a>, <a href="/search/astro-ph?searchtype=author&query=Gronwall%2C+C">C. Gronwall</a>, <a href="/search/astro-ph?searchtype=author&query=Infante%2C+L">L. Infante</a>, <a href="/search/astro-ph?searchtype=author&query=Kimble%2C+R+A">R. A. Kimble</a>, <a href="/search/astro-ph?searchtype=author&query=Krist%2C+J">J. Krist</a>, <a href="/search/astro-ph?searchtype=author&query=Lesser%2C+M">M. Lesser</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0211371v1-abstract-short" style="display: inline;"> We present the first Advanced Camera for Surveys (ACS) observations of young star clusters in the colliding/merging galaxy UGC 10214. The observations were made as part of the Early Release Observation (ERO) program for the newly installed ACS during service mission SM3B for the Hubble Space Telescope (HST). Many young star clusters can be identified in the tails of UGC 10214, with ages ranging… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0211371v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0211371v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0211371v1-abstract-full" style="display: none;"> We present the first Advanced Camera for Surveys (ACS) observations of young star clusters in the colliding/merging galaxy UGC 10214. The observations were made as part of the Early Release Observation (ERO) program for the newly installed ACS during service mission SM3B for the Hubble Space Telescope (HST). Many young star clusters can be identified in the tails of UGC 10214, with ages ranging from ~3 Myr to 10 Myr. The extreme blue V-I (F606W-F814W) colors of the star clusters found in the tail of UGC 10214 can only be explained if strong emission lines are included with a young stellar population. This has been confirmed by our Keck spectroscopy of some of these bright blue stellar knots. The most luminous and largest of these blue knots has an absolute magnitude of M_V = -14.45, with a half-light radius of 161 pc, and if it is a single star cluster, would qualify as a super star cluster (SSC). Alternatively, it could be a superposition of multiple scaled OB associations or clusters. With an estimated age of ~ 4-5 Myr, its derived mass is < 1.3 x 10^6 solar masses. Thus the young stellar knot is unbound and will not evolve into a normal globular cluster. The bright blue clusters and associations are much younger than the dynamical age of the tail, providing strong evidence that star formation occurs in the tail long after it was ejected. UGC 10214 provides a nearby example of processes that contributed to the formation of halos and intra-cluster media in the distant and younger Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0211371v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0211371v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 November, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2002. </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 with embedded figures, ApJ in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 585 (2003) 750-755 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0202035">arXiv:astro-ph/0202035</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0202035">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0202035">ps</a>, <a href="https://arxiv.org/format/astro-ph/0202035">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/339846">10.1086/339846 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The nuclei of radio galaxies in the UV: the signature of different emission processes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chiaberge%2C+M">Marco Chiaberge</a>, <a href="/search/astro-ph?searchtype=author&query=Macchetto%2C+F+D">F. Duccio Macchetto</a>, <a href="/search/astro-ph?searchtype=author&query=Sparks%2C+W+B">William B. Sparks</a>, <a href="/search/astro-ph?searchtype=author&query=Capetti%2C+A">Alessandro Capetti</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+M+G">Mark G. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre' R. Martel</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="astro-ph/0202035v1-abstract-short" style="display: inline;"> We have studied the nuclei of 28 radio galaxies from the 3CR sample in the UV band. Unresolved nuclei (central compact cores, CCC) are observed in 10 of the 13 FR I, and in 5 of the 15 FR II. All sources that do not have a CCC in the optical, do not have a CCC in the UV. Two FR I (3C 270 and 3C 296) have a CCC in the optical but do not show the UV counterpart. Both of them show large dusty disks… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0202035v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0202035v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0202035v1-abstract-full" style="display: none;"> We have studied the nuclei of 28 radio galaxies from the 3CR sample in the UV band. Unresolved nuclei (central compact cores, CCC) are observed in 10 of the 13 FR I, and in 5 of the 15 FR II. All sources that do not have a CCC in the optical, do not have a CCC in the UV. Two FR I (3C 270 and 3C 296) have a CCC in the optical but do not show the UV counterpart. Both of them show large dusty disks observed almost edge-on, possibly implying that they play a role in obscuring the nuclear emission. We have measured optical-UV spectral indices alpha_o,UV between ~0.6 and ~7.0. BLRG have the flattest spectra and their values of alpha_o,UV are also confined to a very narrow range. This is consistent with radiation produced in a geometrically thin, optically thick accretion disk. On the other hand, FR I nuclei, which are most plausibly originated by synchrotron emission from the inner relativistic jet, show a wide range of alpha_o,UV. There is a clear trend with orientation in that sources observed almost edge-on or with clear signs of dust absorption have the steepest spectra. These observations imply that in FR I obscuration can be present, but the obscuring material is not in a ``standard'' geometrically thick torus. The most striking difference between these absorbing structures and the classic AGN ``tori'' resides in the lower optical depth of the FR I obscuring material. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0202035v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0202035v1-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 February, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2002. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 4 figures, accepted for publication on 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/astro-ph/0112208">arXiv:astro-ph/0112208</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0112208">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0112208">ps</a>, <a href="https://arxiv.org/format/astro-ph/0112208">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/338823">10.1086/338823 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ultraviolet HST Snapshot Survey of 3CR Radio Source Counterparts at Low Redshift </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Allen%2C+M+G">Mark G. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Sparks%2C+W+B">William B. Sparks</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A">Anton Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=O%27dea%2C+C+P">Christopher P. O'dea</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">Stefi A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Chiaberge%2C+M">Marco Chiaberge</a>, <a href="/search/astro-ph?searchtype=author&query=Macchetto%2C+F+D">F. Duccio Macchetto</a>, <a href="/search/astro-ph?searchtype=author&query=Miley%2C+G+K">George K. Miley</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="astro-ph/0112208v1-abstract-short" style="display: inline;"> We present ultraviolet images of 27 3CR radio galaxies with redshifts z<0.1 that have been imaged with the Space Telescope Imaging Spectrograph (STIS) on board the Hubble Space Telescope (HST). The observations employed the NUV-MAMA and broad-band filters with peak sensitivity at 2200A . We find that the UV luminosities show approximately a factor of 10 to 100 higher dispersion than the optical.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0112208v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0112208v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0112208v1-abstract-full" style="display: none;"> We present ultraviolet images of 27 3CR radio galaxies with redshifts z<0.1 that have been imaged with the Space Telescope Imaging Spectrograph (STIS) on board the Hubble Space Telescope (HST). The observations employed the NUV-MAMA and broad-band filters with peak sensitivity at 2200A . We find that the UV luminosities show approximately a factor of 10 to 100 higher dispersion than the optical. We compare the UV morphologies with optical V- and R-band WFPC2 snapshot survey images. We have found dramatic, complex and extended ultraviolet emission from radio galaxies even at zero redshift. We find a diverse range of UV morphologies, some completely divergent from their visual morphology, which are reminiscent of the chaotic high-z radio galaxies structures seen in rest-frame UV. The UV morphologies show regions of star formation, jets, and possible scattered AGN continuum. The UV emission is generally not aligned with the radio structure. We also detect the diffuse UV emission of the host galaxy. We propose that these are the same physical phenomena as observed at high redshift, but on a smaller spatial scale. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0112208v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0112208v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2001. </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">Version with high resolution images available at http://www.stsci.edu/~mga/pp.pdf Accepted ApJ supplements November 21, 2001</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0110409">arXiv:astro-ph/0110409</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0110409">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0110409">ps</a>, <a href="https://arxiv.org/format/astro-ph/0110409">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/324604">10.1086/324604 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Filaments and Ionized Gas in the Vicinity of 3C 244.1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">Carlos Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Macchetto%2C+F+D">F. Duccio Macchetto</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Sparks%2C+W+B">William B. Sparks</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="astro-ph/0110409v1-abstract-short" style="display: inline;"> We present results of Hubble Space Telescope observations of the radio galaxy 3C 244.1. The broadband F702W (R) and F555W (V) images (WFPC2/PC) show an elliptical galaxy and gaseous filaments and blobs surrounding it. In the narrow-band ramp filter, dominated by [OIII]lambda5007, these filaments are bright and have the same morphology as the broad band images. To the south, the filaments have a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0110409v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0110409v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0110409v1-abstract-full" style="display: none;"> We present results of Hubble Space Telescope observations of the radio galaxy 3C 244.1. The broadband F702W (R) and F555W (V) images (WFPC2/PC) show an elliptical galaxy and gaseous filaments and blobs surrounding it. In the narrow-band ramp filter, dominated by [OIII]lambda5007, these filaments are bright and have the same morphology as the broad band images. To the south, the filaments have a cone-shaped structure and the radio jet is located at the center of this cone. To the north of the galaxy, the structure is found near the nucleus of the galaxy within its elliptical profile. From the photometry, the two brighter structures seem to be extended narrow line emission regions (ENLRs). The comparison with diagnostic line ratios shows that the observed emission is consistent with interactions between the expanding radio-jet and the local denser medium. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0110409v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0110409v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2001. </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 and 3 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0106168">arXiv:astro-ph/0106168</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0106168">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0106168">ps</a>, <a href="https://arxiv.org/format/astro-ph/0106168">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> Spectropolarimetry of Broad H_alpha Lines and Geometry of the BLR </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+M+H">Marshall H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre' R. Martel</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="astro-ph/0106168v1-abstract-short" style="display: inline;"> In a small fraction of Broad Line Radio Galaxies (BLRG) and Seyfert 1 galaxies, the polarization position angle rotates across the broad emission lines, especially at H_alpha. An understanding of this behavior can potentially yield important information on the scattering geometry in the nucleus. We show two examples of this phenomenon, 3C 445, a BLRG, and Mrk 231, a Seyfert 1, and present an equ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0106168v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0106168v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0106168v1-abstract-full" style="display: none;"> In a small fraction of Broad Line Radio Galaxies (BLRG) and Seyfert 1 galaxies, the polarization position angle rotates across the broad emission lines, especially at H_alpha. An understanding of this behavior can potentially yield important information on the scattering geometry in the nucleus. We show two examples of this phenomenon, 3C 445, a BLRG, and Mrk 231, a Seyfert 1, and present an equatorial scattering model that explains some of its features in a straightforward way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0106168v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0106168v1-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 June, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2001. </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, 3 figures. To appear in Mass Outflow in Active Galactic Nuclei; New Perspectives, Eds D.M. Crenshaw, S.B. Kraemer, and I.M. George</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0101441">arXiv:astro-ph/0101441</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0101441">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0101441">ps</a>, <a href="https://arxiv.org/format/astro-ph/0101441">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/319953">10.1086/319953 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 3C236: Radio Source, Interrupted? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=O%27Dea%2C+C+P">Christopher P. O'Dea</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">Stefi A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Sparks%2C+W+B">William B. Sparks</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+M+G">Mark G. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Macchetto%2C+F+D">Ferdinando D. Macchetto</a>, <a href="/search/astro-ph?searchtype=author&query=Miley%2C+G+K">George K. Miley</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="astro-ph/0101441v1-abstract-short" style="display: inline;"> We present new HST STIS/MAMA near-UV images and archival WFPC2 V and R band images which reveal the presence of four star forming regions in an arc along the edge of the dust lane in the giant (4 Mpc) radio galaxy 3C236. Two of the star forming regions are relatively young with ages of order 1E7 yr, while the other two are older with ages of order 1E8 - 1E9 yr which is comparable to the estimate… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0101441v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0101441v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0101441v1-abstract-full" style="display: none;"> We present new HST STIS/MAMA near-UV images and archival WFPC2 V and R band images which reveal the presence of four star forming regions in an arc along the edge of the dust lane in the giant (4 Mpc) radio galaxy 3C236. Two of the star forming regions are relatively young with ages of order 1E7 yr, while the other two are older with ages of order 1E8 - 1E9 yr which is comparable to the estimated age of the giant radio source. Based on dynamical and spectral aging arguments, we suggest that the fuel supply to the AGN was interrupted for 1E7 yr and has now been restored, resulting in the formation of the inner 2 kpc scale radio source. This time scale is similar to that of the age of the youngest of the star forming regions. We suggest that the transport of gas in the disk is non-steady and that this produces both the multiple episodes of star formation in the disk as well as the multiple epochs of radio source activity. If the inner radio source and the youngest star forming region are related by the same event of gas transport, the gas must be transported from the hundreds of pc scale to the sub-parsec scale on a time scale of 1E7 yr, which is similar to the dynamical time scale of the gas on the hundreds of pc scales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0101441v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0101441v1-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 January, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2001. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0007358">arXiv:astro-ph/0007358</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0007358">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0007358">ps</a>, <a href="https://arxiv.org/format/astro-ph/0007358">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/317064">10.1086/317064 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Face-on Dust Disks in Galaxies with Optical Jets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sparks%2C+W+B">William B. Sparks</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">Stefi A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Biretta%2C+J">John Biretta</a>, <a href="/search/astro-ph?searchtype=author&query=Macchetto%2C+F+D">F. Duccio Macchetto</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre' R. Martel</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="astro-ph/0007358v1-abstract-short" style="display: inline;"> The presence of optical synchrotron jets in radio galaxies is relatively rare. Here, we show that of the nearest five FR-I 3CR radio galaxies showing optical jets, {\it four} show evidence for almost circular, presumably face-on, dust disks. This is strong support for the two-fold idea that (\romannumeral1) jets emerge close to perpendicular to inner gas disks and (\romannumeral2) optical non-th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0007358v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0007358v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0007358v1-abstract-full" style="display: none;"> The presence of optical synchrotron jets in radio galaxies is relatively rare. Here, we show that of the nearest five FR-I 3CR radio galaxies showing optical jets, {\it four} show evidence for almost circular, presumably face-on, dust disks. This is strong support for the two-fold idea that (\romannumeral1) jets emerge close to perpendicular to inner gas disks and (\romannumeral2) optical non-thermal synchrotron emission is seen only when the jet points towards the observer. The implied critical angle to the line-of-sight is approximately 30 - $40^{\circ}$, i.e. if the angle of the jet to the line-of-sight is less than about $40^{\circ}$ we see an optical jet. The corresponding relativisitic $纬$ factor is $\approx 1.5$ which is consistent with current observations of jet proper motion that show a range up to $纬\sim 6$ for M87. The relatively low speeds implied by $纬\approx 1.5$ may be due to a global deceleration of the jet as in unified theories, or else to stratification within the jet. Unresolved nuclei are common in the optical. Their luminosities are also consistent with the beaming concept when compared to inclination inferred from the dust lanes. The disk sizes are typically several hundred parsecs, to kiloparsec size. The galaxy with an optical jet that does not show a face-on disk, M87, instead has more complex radial dust and ionized gas filaments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0007358v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0007358v1-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 July, 2000; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2000. </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, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> STScI preprint: 1440 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9911381">arXiv:astro-ph/9911381</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9911381">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9911381">ps</a>, <a href="https://arxiv.org/format/astro-ph/9911381">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/312503">10.1086/312503 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chandra X-Ray Detection of the Radio Hotspots of 3C295 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Harris%2C+D+E">D. E. Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Nulsen%2C+P+E+J">P. E. J. Nulsen</a>, <a href="/search/astro-ph?searchtype=author&query=Ponman%2C+T+P">T. P. Ponman</a>, <a href="/search/astro-ph?searchtype=author&query=Bautz%2C+M">M. Bautz</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+R+A">R. A. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=David%2C+L+P">L. P. David</a>, <a href="/search/astro-ph?searchtype=author&query=Donnelly%2C+R+H">R. H. Donnelly</a>, <a href="/search/astro-ph?searchtype=author&query=Forman%2C+W+R">W. R. Forman</a>, <a href="/search/astro-ph?searchtype=author&query=Grego%2C+L">L. Grego</a>, <a href="/search/astro-ph?searchtype=author&query=Hardcastle%2C+M+J">M. J. Hardcastle</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+J+P">J. P. Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+C">C. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Leahy%2C+J+P">J. P. Leahy</a>, <a href="/search/astro-ph?searchtype=author&query=Markevitch%2C+M">M. Markevitch</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=McNamara%2C+B+R">B. R. McNamara</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzotta%2C+P">P. Mazzotta</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+W">W. Tucker</a>, <a href="/search/astro-ph?searchtype=author&query=Virani%2C+S+N">S. N. Virani</a>, <a href="/search/astro-ph?searchtype=author&query=Vrtilek%2C+J">J. Vrtilek</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="astro-ph/9911381v1-abstract-short" style="display: inline;"> An observation of the radio galaxy 3C295 during the calibration phase of the Chandra X-ray Observatory reveals X-ray emission from the core of the galaxy, from each of the two prominent radio hotspots, and from the previously known cluster gas. We discuss the possible emission processes for the hotspots and argue that a synchrotron self-Compton model is preferred for most or all of the observed… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9911381v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9911381v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9911381v1-abstract-full" style="display: none;"> An observation of the radio galaxy 3C295 during the calibration phase of the Chandra X-ray Observatory reveals X-ray emission from the core of the galaxy, from each of the two prominent radio hotspots, and from the previously known cluster gas. We discuss the possible emission processes for the hotspots and argue that a synchrotron self-Compton model is preferred for most or all of the observed X-ray emission. SSC models with near equipartition fields thus explain the X-ray emission from the hotspots in the two highest surface brightness FRII radio galaxies, Cygnus A and 3C295. This lends weight to the assumption of equipartition and suggests that relativistic protons do not dominate the particle energy density. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9911381v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9911381v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 November, 1999; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 1999. </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, 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/astro-ph/9906059">arXiv:astro-ph/9906059</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9906059">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9906059">ps</a>, <a href="https://arxiv.org/format/astro-ph/9906059">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/308030">10.1086/308030 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Extended Line Region of 3C 299 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">Carlos Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Macchetto%2C+F+D">F. Duccio Macchetto</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Sparks%2C+W+B">William B. Sparks</a>, <a href="/search/astro-ph?searchtype=author&query=McCarthy%2C+P+J">Patrick J. McCarthy</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="astro-ph/9906059v1-abstract-short" style="display: inline;"> We present results of HST observations of the radio galaxy 3C 299. The broad-band F702W (R) and F555W (V) images (WFPC2/PC) show an elliptical galaxy, with a comet-like structure extending to the NE in the radio jet direction. The [OIII]$位$5007 emission line map, shows a bi-conical structure centered on the nucleus, that overlaps the structure found in the broad-band filters. The radio core coin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9906059v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9906059v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9906059v1-abstract-full" style="display: none;"> We present results of HST observations of the radio galaxy 3C 299. The broad-band F702W (R) and F555W (V) images (WFPC2/PC) show an elliptical galaxy, with a comet-like structure extending to the NE in the radio jet direction. The [OIII]$位$5007 emission line map, shows a bi-conical structure centered on the nucleus, that overlaps the structure found in the broad-band filters. The radio core coincides with the center of the bi-conical structure and the radio axes are aligned with the direction of the cones. These data show clear evidence of a strong interaction between the radio jet and the NE morphology of the galaxy. We show evidence that this NE region is an ENLR; the line-ratio diagnostics show that models involving gas shocked by the radio-jet plus ionization from a precursor HII region, produced itself by the ionizing photons of the postshocked gas on the preshocked gas provide a good match to the observations. We investigate the spatial behavior of the ionizing parameter $U$, by determining the [OIII]/[OII] line ratio which is sensitive to the change of the ionization parameter, and trace its behavior over the ENLR along the radio jet direction. We find that [OIII]/[OII] does not follow a simple dilution model, but rather that it is approximately constant over a large range of distance from the nucleus thus requiring a local source of ionization which seems to be compatible with the shock models driven by the radio jet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9906059v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9906059v1-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 June, 1999; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 1999. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 9 Postscript figures, ApJ accepted, uses aaspp.sty</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9905299">arXiv:astro-ph/9905299</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9905299">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9905299">ps</a>, <a href="https://arxiv.org/format/astro-ph/9905299">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/313272">10.1086/313272 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Polarization of Broad Absorption Line QSOs I. A Spectropolarimetric Atlas </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ogle%2C+P+M">P. M. Ogle</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+M+H">M. H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+J+S">J. S. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Tran%2C+H+D">H. D. Tran</a>, <a href="/search/astro-ph?searchtype=author&query=Goodrich%2C+R+W">R. W. Goodrich</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">A. R. Martel</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="astro-ph/9905299v1-abstract-short" style="display: inline;"> We present a spectropolarimetric survey of 36 broad absorption line quasi-stellar objects (BAL QSOs). The continuum, absorption trough, and emission line polarization of BAL QSOs yield clues about their structure. We confirm that BAL QSOs are in general more highly polarized than non-BAL QSOs, consistent with a more equatorial viewing direction for the former than the latter. We have identified… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9905299v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9905299v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9905299v1-abstract-full" style="display: none;"> We present a spectropolarimetric survey of 36 broad absorption line quasi-stellar objects (BAL QSOs). The continuum, absorption trough, and emission line polarization of BAL QSOs yield clues about their structure. We confirm that BAL QSOs are in general more highly polarized than non-BAL QSOs, consistent with a more equatorial viewing direction for the former than the latter. We have identified two new highly-polarized QSOs in our sample (1232+1325 and 1333+2840). The polarization rises weakly to the blue in most objects, perhaps due to scattering and absorption by dust particles. We find that a polarization increase in the BAL troughs is a general property of polarized BAL QSOs, indicating an excess of scattered light relative to direct light, and consistent with the unification of BAL QSOs and non-BAL QSOs. We have also discovered evidence of resonantly scattered photons in the red wing of the C IV broad emission lines of a few objects. In most cases, the broad emission lines have lower polarization and a different position angle than the continuum. The polarization characteristics of low-ionization BAL QSOs are similar to those of high-ionization BAL QSOs, suggesting a similar BAL wind geometry. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9905299v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9905299v1-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, 1999; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 1999. </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, 6 figures (20 .gif files), accepted for publication in The Astrophysical Journal Supplements</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.Suppl. 125 (1999) 1-34 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 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