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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Scolnic%2C+D&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Scolnic%2C+D&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Scolnic%2C+D&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Scolnic%2C+D&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Scolnic%2C+D&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a href="/search/?searchtype=author&query=Scolnic%2C+D&start=200" class="pagination-link " aria-label="Page 5" aria-current="page">5 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.07881">arXiv:2502.07881</a> <span> [<a href="https://arxiv.org/pdf/2502.07881">pdf</a>, <a href="https://arxiv.org/format/2502.07881">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Measuring the Distances to Asteroids from One Observatory in One Night with Upcoming All-Sky Telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fernandes%2C+M+B">Maryann Benny Fernandes</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+E">Erik Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Zhai%2C+C">Chengxing Zhai</a>, <a href="/search/astro-ph?searchtype=author&query=Linder%2C+T">Tyler Linder</a>, <a href="/search/astro-ph?searchtype=author&query=Acevedo%2C+M">Maria Acevedo</a>, <a href="/search/astro-ph?searchtype=author&query=Reichart%2C+D">Daniel Reichart</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="2502.07881v1-abstract-short" style="display: inline;"> Upcoming telescopes like the Vera Rubin Observatory (VRO) and the Argus Array will image large fractions of the sky multiple times per night yielding numerous Near Earth Object (NEO) discoveries. When asteroids are measured with short observation time windows, the dominant uncertainty in orbit construction is due to distance uncertainty to the NEO. One approach to recover distances is from topocen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.07881v1-abstract-full').style.display = 'inline'; document.getElementById('2502.07881v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.07881v1-abstract-full" style="display: none;"> Upcoming telescopes like the Vera Rubin Observatory (VRO) and the Argus Array will image large fractions of the sky multiple times per night yielding numerous Near Earth Object (NEO) discoveries. When asteroids are measured with short observation time windows, the dominant uncertainty in orbit construction is due to distance uncertainty to the NEO. One approach to recover distances is from topocentric parallax, which is a technique that leverages the rotation of the Earth, causing a small but detectable sinusoidal additive signal to the Right Ascension (RA) of the NEO following a period of 1 day. In this paper, we further develop and evaluate this technique to recover distances in as quickly as a single night. We first test the technique on synthetic data of 19 different asteroids ranging from $\sim0.05 \,\text{AU}$ to $\sim2.4 \,\text{AU}$. We modify previous algorithms and quantify the limitations of the method, recovering distances with uncertainties as low as the $\sim1.3\%$ level for more nearby objects ($\lesssim$ 0.3 AU) assuming typical astrometric uncertainties. We then acquire our own observations of two asteroids within a single night with $\sim0.1''$ uncertainties on RA, and we find we are able to recover distances to the $3\%$ level. We forecast likely scenarios with the VRO and the Argus Array with varying levels of astrometric precision and expected pointings per night. Our analysis indicates that distances to NEOs on the scale of $\sim0.5$ AU can be constrained to below the percent level within a single night, depending on spacing of observations from one observatory. In a follow-up paper, we will compare these constraints with synchronous and asynchronous observations from two separate observatories to measure parallax even more efficiently, an exciting and likely possibility over the upcoming decade. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.07881v1-abstract-full').style.display = 'none'; document.getElementById('2502.07881v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitting to the Astronomical Journal, comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.05259">arXiv:2502.05259</a> <span> [<a href="https://arxiv.org/pdf/2502.05259">pdf</a>, <a href="https://arxiv.org/format/2502.05259">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> JAGB 2.0: Improved Constraints on the J-region Asymptotic Giant Branch-based Hubble Constant from an Expanded Sample of JWST Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+S">Siyang Li</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=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</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="2502.05259v2-abstract-short" style="display: inline;"> The J-region Asymptotic Giant Branch (JAGB) is an overdensity of stars in the near-infrared, attributed to carbon-rich asymptotic giant branch stars, and recently used as a standard candle for measuring extragalactic distances and the Hubble constant. Using JWST in Cycle 2, we extend JAGB measurements to 6 hosts of 9 Type Ia supernovae (SNe Ia) (NGC 2525, NGC 3147, NGC 3370, NGC 3447, NGC 5468, an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.05259v2-abstract-full').style.display = 'inline'; document.getElementById('2502.05259v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.05259v2-abstract-full" style="display: none;"> The J-region Asymptotic Giant Branch (JAGB) is an overdensity of stars in the near-infrared, attributed to carbon-rich asymptotic giant branch stars, and recently used as a standard candle for measuring extragalactic distances and the Hubble constant. Using JWST in Cycle 2, we extend JAGB measurements to 6 hosts of 9 Type Ia supernovae (SNe Ia) (NGC 2525, NGC 3147, NGC 3370, NGC 3447, NGC 5468, and NGC 5861), with two at $D \sim 40$ Mpc, all calibrated by the maser host NGC 4258. We investigate the effects of incompleteness and find that we are unable to recover a robust JAGB measurement in one of the two most distant hosts at $R \sim 40$ Mpc, NGC 3147. We compile all JWST JAGB observations in SNe Ia hosts, 15 galaxies hosting 18 SNe Ia, from the SH0ES and CCHP programs and employ all literature measures (mode, mean, median, model). We find no significant mean difference between these distances and those from HST Cepheids, $-0.03\pm0.02$ (stat) $\pm$ 0.05 (sys) mag. We find a difference of 0.11 $\pm$ 0.02 mag between JAGB mode measurements in the CCHP analyses of two fields in NGC 4258, a feature also seen in two SH0ES fields (see field-to-field variations in Li et al. 2024a), indicating significant field-to-field variation of JAGB measurements in NGC 4258 which produce a large absolute calibration uncertainty. Variations are also seen in the shape of the JAGB LF across galaxies so that different measures produce different values of the Hubble constant. We look for but do not (yet) find a standardizing relation between JAGB LF skew or color dependence and the apparent variation. Using the middle result of all JAGB measures to calibrate SNe Ia yields a Hubble constant of $H_0$ = 73.3 $\pm$ 1.4 (stat) $\pm$ 2.0 (sys) km/s/Mpc with the systematic dominated by apparent differences across NGC 4258 calibrating fields or their measures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.05259v2-abstract-full').style.display = 'none'; document.getElementById('2502.05259v2-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 18 figures, 7 tables, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.06664">arXiv:2501.06664</a> <span> [<a href="https://arxiv.org/pdf/2501.06664">pdf</a>, <a href="https://arxiv.org/format/2501.06664">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Comparing the DES-SN5YR and Pantheon+ SN cosmology analyses: Investigation based on "Evolving Dark Energy or Supernovae systematics?" </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Camilleri%2C+R">R. Camilleri</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Rose%2C+B">B. Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a> , et al. (43 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.06664v1-abstract-short" style="display: inline;"> Recent cosmological analyses measuring distances of Type Ia Supernovae (SNe Ia) and Baryon Acoustic Oscillations (BAO) have all given similar hints at time-evolving dark energy. To examine whether underestimated SN Ia systematics might be driving these results, Efstathiou (2024) compared overlapping SN events between Pantheon+ and DES-SN5YR (20% SNe are in common), and reported evidence for a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.06664v1-abstract-full').style.display = 'inline'; document.getElementById('2501.06664v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.06664v1-abstract-full" style="display: none;"> Recent cosmological analyses measuring distances of Type Ia Supernovae (SNe Ia) and Baryon Acoustic Oscillations (BAO) have all given similar hints at time-evolving dark energy. To examine whether underestimated SN Ia systematics might be driving these results, Efstathiou (2024) compared overlapping SN events between Pantheon+ and DES-SN5YR (20% SNe are in common), and reported evidence for a $\sim$0.04 mag offset between the low and high-redshift distance measurements of this subsample of events. If these offsets are arbitrarily subtracted from the entire DES-SN5YR sample, the preference for evolving dark energy is reduced. In this paper, we reproduce this offset and show that it has two sources. First, 43% of the offset is due to DES-SN5YR improvements in the modelling of supernova intrinsic scatter and host galaxy properties. These are scientifically-motivated modelling updates implemented in DES-SN5YR and their associated uncertainties are captured within the DES-SN5YR systematic error budget. Even if the less accurate scatter model and host properties from Pantheon+ are used instead, the DES-SN5YR evidence for evolving dark energy is only reduced from 3.9$蟽$ to 3.3$蟽$. Second, 38% of the offset is due to a misleading comparison because different selection functions characterize the DES subsets included in Pantheon+ and DES-SN5YR and therefore individual SN distance measurements are expected to be different because of different bias corrections. In conclusion, we confirm the validity of the published DES-SN5YR results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.06664v1-abstract-full').style.display = 'none'; document.getElementById('2501.06664v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.05632">arXiv:2501.05632</a> <span> [<a href="https://arxiv.org/pdf/2501.05632">pdf</a>, <a href="https://arxiv.org/format/2501.05632">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> OpenUniverse2024: A shared, simulated view of the sky for the next generation of cosmological surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=OpenUniverse"> OpenUniverse</a>, <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+L+D+E+S">The LSST Dark Energy Science Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Team%2C+T+R+H+P+I">The Roman HLIS Project Infrastructure Team</a>, <a href="/search/astro-ph?searchtype=author&query=Team%2C+T+R+R+P+I">The Roman RAPID Project Infrastructure Team</a>, <a href="/search/astro-ph?searchtype=author&query=Team%2C+T+R+S+C+P+I">The Roman Supernova Cosmology Project Infrastructure Team</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</a>, <a href="/search/astro-ph?searchtype=author&query=Aldoroty%2C+L">L. Aldoroty</a>, <a href="/search/astro-ph?searchtype=author&query=Beltz-Mohrmann%2C+G">G. Beltz-Mohrmann</a>, <a href="/search/astro-ph?searchtype=author&query=Bera%2C+A">A. Bera</a>, <a href="/search/astro-ph?searchtype=author&query=Blazek%2C+J">J. Blazek</a>, <a href="/search/astro-ph?searchtype=author&query=Bogart%2C+J">J. Bogart</a>, <a href="/search/astro-ph?searchtype=author&query=Braeunlich%2C+G">G. Braeunlich</a>, <a href="/search/astro-ph?searchtype=author&query=Broughton%2C+A">A. Broughton</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+K">K. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+J">J. Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Chisari%2C+N+E">N. E. Chisari</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+V">V. Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+Y">Y. Fang</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Hearin%2C+A">A. Hearin</a>, <a href="/search/astro-ph?searchtype=author&query=Heitmann%2C+K">K. Heitmann</a>, <a href="/search/astro-ph?searchtype=author&query=Hirata%2C+C">C. Hirata</a>, <a href="/search/astro-ph?searchtype=author&query=Hounsell%2C+R">R. Hounsell</a>, <a href="/search/astro-ph?searchtype=author&query=Jain%2C+B">B. Jain</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M">M. Jarvis</a> , et al. (35 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.05632v1-abstract-short" style="display: inline;"> The OpenUniverse2024 simulation suite is a cross-collaboration effort to produce matched simulated imaging for multiple surveys as they would observe a common simulated sky. Both the simulated data and associated tools used to produce it are intended to uniquely enable a wide range of studies to maximize the science potential of the next generation of cosmological surveys. We have produced simulat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05632v1-abstract-full').style.display = 'inline'; document.getElementById('2501.05632v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.05632v1-abstract-full" style="display: none;"> The OpenUniverse2024 simulation suite is a cross-collaboration effort to produce matched simulated imaging for multiple surveys as they would observe a common simulated sky. Both the simulated data and associated tools used to produce it are intended to uniquely enable a wide range of studies to maximize the science potential of the next generation of cosmological surveys. We have produced simulated imaging for approximately 70 deg$^2$ of the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) Wide-Fast-Deep survey and the Nancy Grace Roman Space Telescope High-Latitude Wide-Area Survey, as well as overlapping versions of the ELAIS-S1 Deep-Drilling Field for LSST and the High-Latitude Time-Domain Survey for Roman. OpenUniverse2024 includes i) an early version of the updated extragalactic model called Diffsky, which substantially improves the realism of optical and infrared photometry of objects, compared to previous versions of these models; ii) updated transient models that extend through the wavelength range probed by Roman and Rubin; and iii) improved survey, telescope, and instrument realism based on up-to-date survey plans and known properties of the instruments. It is built on a new and updated suite of simulation tools that improves the ease of consistently simulating multiple observatories viewing the same sky. The approximately 400 TB of synthetic survey imaging and simulated universe catalogs are publicly available, and we preview some scientific uses of the simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05632v1-abstract-full').style.display = 'none'; document.getElementById('2501.05632v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.08449">arXiv:2412.08449</a> <span> [<a href="https://arxiv.org/pdf/2412.08449">pdf</a>, <a href="https://arxiv.org/format/2412.08449">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Calibrating the Tully-Fisher Relation to Measure the Hubble Constant </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Boubel%2C+P">Paula Boubel</a>, <a href="/search/astro-ph?searchtype=author&query=Byrne%2C+J">Jakob Byrne</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=Anand%2C+G+S">Gagandeep S. Anand</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="2412.08449v1-abstract-short" style="display: inline;"> Boubel et al. 2024 (B24) recently used the Tully-Fisher (TF) relation to measure calibrated distances in the Hubble flow and found $H_0= 73.3 \pm 2.1 (stat) \pm 3.5 (sys)$ km/s/Mpc. The large systematic uncertainty was the result of propagating the conflict between two sources of empirical distance calibration: a difference in zeropoint when calibrating the TF relation with Type Ia supernovae (SNe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.08449v1-abstract-full').style.display = 'inline'; document.getElementById('2412.08449v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.08449v1-abstract-full" style="display: none;"> Boubel et al. 2024 (B24) recently used the Tully-Fisher (TF) relation to measure calibrated distances in the Hubble flow and found $H_0= 73.3 \pm 2.1 (stat) \pm 3.5 (sys)$ km/s/Mpc. The large systematic uncertainty was the result of propagating the conflict between two sources of empirical distance calibration: a difference in zeropoint when calibrating the TF relation with Type Ia supernovae (SNe Ia) versus Cepheids and Tip-of-the-Red-Giant-Branch (TRGB) and an apparent difference in zeropoint between two distinct TRGB datasets. We trace the SN Ia-based calibration used in the TF analysis to a study where $H_0$ was fixed to 70 km/s/Mpc rather than measured, (with host distances derived from redshifts and the Hubble law), thus introducing a discrepancy with the other empirically calibrated indicators. In addition, we trace the difference in TRGB zeropoints to a miscalibration of $0.14$ mag that should be $\sim0.01-0.04$ mag. Using the consistent Cepheid and TRGB calibration from B24 while removing the problematic data reduces the systematic error by a factor of two and results in $H_0 = 76.3 \pm 2.1 \textrm{(stat)} \pm 1.5 \textrm{(sys)}$ km/s/Mpc. This measurement is consistent with previous determinations of $H_0$ using the TF relation. We also show that most determinations of $H_0$ measurements that replace Type Ia supernovae measurements with another far-field distance indicator yield $H_0>73$ km/s/Mpc, reinforcing previous findings that the Hubble tension is not tied to any one distance indicator. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.08449v1-abstract-full').style.display = 'none'; document.getElementById('2412.08449v1-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Comments very welcome. Submitting to Research Notes of the AAS next week</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.15140">arXiv:2410.15140</a> <span> [<a href="https://arxiv.org/pdf/2410.15140">pdf</a>, <a href="https://arxiv.org/format/2410.15140">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> PS1-11aop: Probing the Mass Loss History of a Luminous Interacting Supernova Prior to its Final Eruption with Multi-wavelength Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ibik%2C+A+L">Adaeze L. Ibik</a>, <a href="/search/astro-ph?searchtype=author&query=Drout%2C+M+R">Maria R. Drout</a>, <a href="/search/astro-ph?searchtype=author&query=Margutti%2C+R">Raffaela Margutti</a>, <a href="/search/astro-ph?searchtype=author&query=Matthews%2C+D">David Matthews</a>, <a href="/search/astro-ph?searchtype=author&query=Villar%2C+V+A">V. Ashley Villar</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+E">Edo Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Chornock%2C+R">Ryan Chornock</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+K+D">Kate D. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Eftekhari%2C+T">Tarraneh Eftekhari</a>, <a href="/search/astro-ph?searchtype=author&query=Laskar%2C+T">Tanmoy Laskar</a>, <a href="/search/astro-ph?searchtype=author&query=Lunnan%2C+R">Ragnhild Lunnan</a>, <a href="/search/astro-ph?searchtype=author&query=Foley%2C+R+J">Ryan J. Foley</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D">David Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Milisavljevic%2C+D">Dan Milisavljevic</a>, <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">Armin Rest</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+P+K+G">Peter K. G. Williams</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="2410.15140v1-abstract-short" style="display: inline;"> Luminous interacting supernovae are a class of stellar explosions whose progenitors underwent vigorous mass loss in the years prior to core-collapse. While the mechanism by which this material is ejected is still debated, obtaining the full density profile of the circumstellar medium (CSM) could reveal more about this process. Here, we present an extensive multi-wavelength study of PS1-11aop, a lu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.15140v1-abstract-full').style.display = 'inline'; document.getElementById('2410.15140v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.15140v1-abstract-full" style="display: none;"> Luminous interacting supernovae are a class of stellar explosions whose progenitors underwent vigorous mass loss in the years prior to core-collapse. While the mechanism by which this material is ejected is still debated, obtaining the full density profile of the circumstellar medium (CSM) could reveal more about this process. Here, we present an extensive multi-wavelength study of PS1-11aop, a luminous and slowly declining Type IIn SN discovered by the PanSTARRS Medium Deep Survey. PS1-11aop had a peak r-band magnitude of $-$20.5\,mag, a total radiated energy $>$ 8$\times$10$^{50}$\,erg, and it exploded near the center of a star-forming galaxy with super-solar metallicity. We obtained multiple detections at the location of PS1-11aop in the radio and X-ray bands between 4 and 10\,years post-explosion, and if due to the SN, it is one of the most luminous radio supernovae identified to date. Taken together, the multiwavelength properties of PS1-11aop are consistent with a CSM density profile with multiple zones. The early optical emission is consistent with the supernova blastwave interacting with a dense and confined CSM shell which contains multiple solar masses of material that was likely ejected in the final $<$10-100 years prior to the explosion,($\sim$0.05$-$1.0 M$_{\odot}$yr$^{-1}$ at radii of $\lesssim$10$^{16}$\,cm). The radio observations, on the other hand, are consistent with a sparser environment ($\lesssim$2$\times 10^{-3}$ M$_{\odot}$yr$^{-1}$ at radii of $\sim$0.5-1$\times$10$^{17}$\,cm) -- thus probing the history of the progenitor star prior to its final mass loss episode. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.15140v1-abstract-full').style.display = 'none'; document.getElementById('2410.15140v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages, 17 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/2409.14546">arXiv:2409.14546</a> <span> [<a href="https://arxiv.org/pdf/2409.14546">pdf</a>, <a href="https://arxiv.org/format/2409.14546">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Hubble Tension in our own Backyard: DESI and the Nearness of the Coma Cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</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=Murakami%2C+Y+S">Yukei S. Murakami</a>, <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+E+R">Erik R. Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">Dillon Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Acevedo%2C+M">Maria Acevedo</a>, <a href="/search/astro-ph?searchtype=author&query=Carreres%2C+B">Bastien Carreres</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+O">David O. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Said%2C+K">Khaled Said</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">Cullan Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</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="2409.14546v2-abstract-short" style="display: inline;"> The Dark Energy Spectroscopic Instrument (DESI) collaboration measured a tight relation between the Hubble constant ($H_0$) and the distance to the Coma cluster using the fundamental plane (FP) relation of the deepest, most homogeneous sample of early-type galaxies. To determine $H_0$, we measure the distance to Coma by several independent routes each with its own geometric reference. We measure t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.14546v2-abstract-full').style.display = 'inline'; document.getElementById('2409.14546v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.14546v2-abstract-full" style="display: none;"> The Dark Energy Spectroscopic Instrument (DESI) collaboration measured a tight relation between the Hubble constant ($H_0$) and the distance to the Coma cluster using the fundamental plane (FP) relation of the deepest, most homogeneous sample of early-type galaxies. To determine $H_0$, we measure the distance to Coma by several independent routes each with its own geometric reference. We measure the most precise distance to Coma from 12 Type Ia Supernovae (SNe Ia) in the cluster with mean standardized brightness of $m_B^0=15.712\pm0.041$ mag. Calibrating the absolute magnitude of SNe Ia with the HST distance ladder yields $D_{\textrm Coma}=98.5\pm2.2$ Mpc, consistent with its canonical value of 95--100 Mpc. This distance results in $H_0=76.5 \pm 2.2$ km/s/Mpc from the DESI FP relation. Inverting the DESI relation by calibrating it instead to the Planck+$螞$CDM value of $H_0=67.4$ km/s/Mpc implies a much greater distance to Coma, $D_{\textrm Coma}=111.8\pm1.8$ Mpc, $4.6蟽$ beyond a joint, direct measure. Independent of SNe Ia, the HST Key Project FP relation as calibrated by Cepheids, Tip of the Red Giant Branch from JWST, or HST NIR surface brightness fluctuations all yield $D_{\textrm Coma}<$ 100 Mpc, in joint tension themselves with the Planck-calibrated route at $>3蟽$. From a broad array of distance estimates compiled back to 1990, it is hard to see how Coma could be located as far as the Planck+$螞$CDM expectation of $>$110 Mpc. By extending the Hubble diagram to Coma, a well-studied location in our own backyard whose distance was in good accord well before the Hubble Tension, DESI indicates a more pervasive conflict between our knowledge of local distances and cosmological expectations. We expect future programs to refine the distance to Coma and nearer clusters to help illuminate this new, local window on the Hubble Tension. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.14546v2-abstract-full').style.display = 'none'; document.getElementById('2409.14546v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">v2 - team name fixed</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.14560">arXiv:2408.14560</a> <span> [<a href="https://arxiv.org/pdf/2408.14560">pdf</a>, <a href="https://arxiv.org/format/2408.14560">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ada285">10.3847/1538-4357/ada285 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improving the Determination of Supernova Cosmological Redshifts by Using Galaxy Groups </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+E+R">Erik R. Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Carreres%2C+B">Bastien Carreres</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+A">Anthony Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+A">Ava Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">Tamara M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">Dillon Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">Cullan Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+O">David O. Jones</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=Said%2C+K">Khaled Said</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+G">Georgie Taylor</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.14560v2-abstract-short" style="display: inline;"> At the low-redshift end ($z<0.05$) of the Hubble diagram with Type Ia Supernovae (SNe Ia), the contribution to Hubble residual scatter from peculiar velocities is of similar size to that due to the limitations of the standardization of the SN Ia light curves. A way to improve the redshift measurement of the SN host galaxy is to utilize the average redshift of the galaxy group, effectively averagin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.14560v2-abstract-full').style.display = 'inline'; document.getElementById('2408.14560v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.14560v2-abstract-full" style="display: none;"> At the low-redshift end ($z<0.05$) of the Hubble diagram with Type Ia Supernovae (SNe Ia), the contribution to Hubble residual scatter from peculiar velocities is of similar size to that due to the limitations of the standardization of the SN Ia light curves. A way to improve the redshift measurement of the SN host galaxy is to utilize the average redshift of the galaxy group, effectively averaging over small-scale/intracluster peculiar velocities. One limiting factor is the fraction of SN host galaxies in galaxy groups, previously found to be 30% using (relatively incomplete) magnitude-limited galaxy catalogs. Here, we do the first analysis of N-body simulations to predict this fraction, finding $\sim$73% should have associated groups and group averaging should improve redshift precision by $\sim$135 km s$^{-1}$ ($\sim$0.04 mag at $z=0.025$). Furthermore, using spectroscopic data from the Anglo-Australian Telescope, we present results from the first pilot program to evaluate whether or not 23 previously unassociated SN Ia hosts belong in groups. We find that 91% of these candidates can be associated with groups, consistent with predictions from simulations given the sample size. Combining with previously assigned SN host galaxies in Pantheon+, we demonstrate improvement in Hubble residual scatter equivalent to 145 km s$^{-1}$, also consistent with simulations. For new and upcoming low-$z$ samples from, for example, ZTF and LSST, a separate follow-up program identifying galaxy groups of SN hosts is a highly cost-effective way to enhance their constraining power. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.14560v2-abstract-full').style.display = 'none'; document.getElementById('2408.14560v2-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 12 figures. Published 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/2408.11770">arXiv:2408.11770</a> <span> [<a href="https://arxiv.org/pdf/2408.11770">pdf</a>, <a href="https://arxiv.org/format/2408.11770">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> JWST Validates HST Distance Measurements: Selection of Supernova Subsample Explains Differences in JWST Estimates of Local H0 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Breuval%2C+L">Louise Breuval</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Macri%2C+L+M">Lucas M. Macri</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+S">Siyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Wenlong Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+C+D">Caroline D. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Jha%2C+S">Saurabh Jha</a>, <a href="/search/astro-ph?searchtype=author&query=Murakami%2C+Y+S">Yukei S. Murakami</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachael Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">Dillon Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+T">Tianrui Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Addison%2C+G+E">Graeme E. Addison</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+C">Charles Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Filippenko%2C+A+V">Alexei V. Filippenko</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+A">Anthony Carr</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.11770v2-abstract-short" style="display: inline;"> JWST provides new opportunities to cross-check the HST Cepheid/SNeIa distance ladder, which yields the most precise local measure of H0. We analyze early JWST subsamples (~1/4 of the HST sample) from the SH0ES and CCHP groups, calibrated by a single anchor (N4258). We find HST Cepheid distances agree well (~1 sigma) with all 8 combinations of methods, samples, and telescopes: JWST Cepheids, TRGB,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.11770v2-abstract-full').style.display = 'inline'; document.getElementById('2408.11770v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.11770v2-abstract-full" style="display: none;"> JWST provides new opportunities to cross-check the HST Cepheid/SNeIa distance ladder, which yields the most precise local measure of H0. We analyze early JWST subsamples (~1/4 of the HST sample) from the SH0ES and CCHP groups, calibrated by a single anchor (N4258). We find HST Cepheid distances agree well (~1 sigma) with all 8 combinations of methods, samples, and telescopes: JWST Cepheids, TRGB, and JAGB by either group, plus HST TRGB and Miras. The comparisons explicitly include the measurement uncertainty of each method in N4258, an oft-neglected but dominant term. Mean differences are ~0.03 mag, far smaller than the 0.18 mag "Hubble tension." Combining all measures produces the strongest constraint yet on the linearity of HST Cepheid distances, 0.994+-0.010, ruling out distance-dependent bias or offset as the source of the tension at ~7 sigma. Yet, measurements of H0 from current JWST subsamples produce large sampling differences whose size and direction we can directly estimate from the full HST set. We show that Delta(H0)~2.5 km/s/Mpc between the CCHP JWST program and the full HST sample is entirely consistent with differences in sample selection. Combining all JWST samples produces a new, distance-limited set of 16 SNeIa at D<25 Mpc and more closely resembles the full sample thanks to "reversion to the mean" of larger samples. Using JWST Cepheids, JAGB, and TRGB, we find 73.4+-2.1, 72.2+-2.2, and 72.1+-2.2 km/s/Mpc, respectively. Explicitly accounting for SNe in common, the combined-sample three-method result from JWST is H0=72.6+-2.0, similar to H0=72.8 expected from HST Cepheids in the same galaxies. The small JWST sample trivially lowers the Hubble tension significance due to small-sample statistics and is not yet competitive with the HST set (42 SNeIa and 4 anchors), which yields 73.2+-0.9. Still, the joint JWST sample provides important crosschecks which the HST data passes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.11770v2-abstract-full').style.display = 'none'; document.getElementById('2408.11770v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ accepted, version replaced with accepted version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.03749">arXiv:2408.03749</a> <span> [<a href="https://arxiv.org/pdf/2408.03749">pdf</a>, <a href="https://arxiv.org/format/2408.03749">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Suppression of the type Ia supernova host galaxy step in the outer regions of galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Toy%2C+M">M. Toy</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Frohmaier%2C+C">C. Frohmaier</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a> , et al. (41 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.03749v1-abstract-short" style="display: inline;"> Using 1533 type Ia supernovae (SNe Ia) from the five-year sample of the Dark Energy Survey (DES), we investigate the effects of projected galactocentric separation between the SNe and their host galaxies on their light curves and standardization. We show, for the first time, that the difference in SN Ia post-standardization brightnesses between high and low-mass hosts reduces from $0.078\pm0.011$… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03749v1-abstract-full').style.display = 'inline'; document.getElementById('2408.03749v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.03749v1-abstract-full" style="display: none;"> Using 1533 type Ia supernovae (SNe Ia) from the five-year sample of the Dark Energy Survey (DES), we investigate the effects of projected galactocentric separation between the SNe and their host galaxies on their light curves and standardization. We show, for the first time, that the difference in SN Ia post-standardization brightnesses between high and low-mass hosts reduces from $0.078\pm0.011$ mag in the full sample to $0.036 \pm 0.018$ mag for SNe Ia located in the outer regions of their host galaxies, while increasing to $0.100 \pm 0.014$ mag for SNe in the inner regions. In these inner regions, the step can be reduced (but not removed) using a model where the $R_V$ of dust along the line-of-sight to the SN changes as a function of galaxy properties. To explain the remaining difference, we use the distributions of the SN Ia stretch parameter to test whether the inferred age of SN progenitors are more varied in the inner regions of galaxies. We find that the proportion of high-stretch SNe Ia in red (older) environments is more prominent in outer regions and that the outer regions stretch distributions are overall more homogeneous compared to inner regions, but conclude that this effect cannot explain the reduction in significance of any Hubble residual step in outer regions. We conclude that the standardized distances of SNe Ia located in the outer regions of galaxies are less affected by their global host galaxy properties than those in the inner regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03749v1-abstract-full').style.display = 'none'; document.getElementById('2408.03749v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 13 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.01001">arXiv:2408.01001</a> <span> [<a href="https://arxiv.org/pdf/2408.01001">pdf</a>, <a href="https://arxiv.org/format/2408.01001">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Calibrating the Absolute Magnitude of Type Ia Supernovae in Nearby Galaxies using [OII] and Implications for $H_{0}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+M">M. Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Mould%2C+J">J. Mould</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+E+N">E. N. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Flynn%2C+C">C. Flynn</a>, <a href="/search/astro-ph?searchtype=author&query=Duffy%2C+A+R">A. R. Duffy</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S+S">S. S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C">C. Conselice</a> , et al. (47 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.01001v2-abstract-short" style="display: inline;"> The present state of cosmology is facing a crisis where there is a fundamental disagreement in measurements of the Hubble constant ($H_{0}$), with significant tension between the early and late universe methods. Type Ia supernovae (SNe Ia) are important to measuring $H_{0}$ through the astronomical distance ladder. However, there remains potential to better standardise SN Ia light curves by using… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.01001v2-abstract-full').style.display = 'inline'; document.getElementById('2408.01001v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.01001v2-abstract-full" style="display: none;"> The present state of cosmology is facing a crisis where there is a fundamental disagreement in measurements of the Hubble constant ($H_{0}$), with significant tension between the early and late universe methods. Type Ia supernovae (SNe Ia) are important to measuring $H_{0}$ through the astronomical distance ladder. However, there remains potential to better standardise SN Ia light curves by using known dependencies on host galaxy properties after the standard light curve width and colour corrections have been applied to the peak SN Ia luminosities. To explore this, we use the 5-year photometrically identified SNe Ia sample obtained by the Dark Energy Survey, along with host galaxy spectra obtained by the Australian Dark Energy Survey. Using host galaxy spectroscopy, we find a significant trend with the equivalent width (EW) of the [OII] $位位$ 3727, 29 doublet, a proxy for specific star formation rate, and Hubble residuals. We find that the correlation with [OII] EW is a powerful alternative to the commonly used mass step after initial light curve corrections. Applying this [OII] EW correction to 20 SNe Ia in calibrator galaxies observed with WiFeS, we examined the impact on SN Ia absolute magnitudes and $H_{0}$. Our [OII] EW corrections result in $H_{0}$ values ranging between 73.04 to 73.51 $\mathrm{km} \mathrm{s}^{-1} \mathrm{Mpc}^{-1}$, with a combined statistical and systematic uncertainty of $\sim$1.31 $\mathrm{km} \mathrm{s}^{-1} \mathrm{Mpc}^{-1}$. However, even with this additional correction, the impact of host galaxy properties in standardising SNe Ia appears limited in reducing the current tension ($\sim$5$蟽$) with the CMB result for $H_{0}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.01001v2-abstract-full').style.display = 'none'; document.getElementById('2408.01001v2-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 13 figures. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.00065">arXiv:2408.00065</a> <span> [<a href="https://arxiv.org/pdf/2408.00065">pdf</a>, <a href="https://arxiv.org/format/2408.00065">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad84f3">10.3847/1538-4357/ad84f3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tip of the Red Giant Branch Distances with JWST. II. I-band Measurements in a Sample of Hosts of 10 SN Ia Match HST Cepheids </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+S">Siyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</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=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Wenlong Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Breuval%2C+L">Louise Breuval</a>, <a href="/search/astro-ph?searchtype=author&query=Macri%2C+L+M">Lucas M. Macri</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachael Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.00065v3-abstract-short" style="display: inline;"> The Hubble Tension, a >5 sigma discrepancy between direct and indirect measurements of the Hubble constant (H0), has persisted for a decade and motivated intense scrutiny of the paths used to infer H0. Comparing independently-derived distances for a set of galaxies with different standard candles, such as the tip of the red giant branch (TRGB) and Cepheid variables, can test for systematics in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.00065v3-abstract-full').style.display = 'inline'; document.getElementById('2408.00065v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.00065v3-abstract-full" style="display: none;"> The Hubble Tension, a >5 sigma discrepancy between direct and indirect measurements of the Hubble constant (H0), has persisted for a decade and motivated intense scrutiny of the paths used to infer H0. Comparing independently-derived distances for a set of galaxies with different standard candles, such as the tip of the red giant branch (TRGB) and Cepheid variables, can test for systematics in the middle rung of the distance ladder. The I band is the preferred filter for measuring the TRGB due to constancy with color, a result of low sensitivity to population differences in age and metallicity supported by stellar models. We use James Webb Space Telescope (JWST) observations with the maser host NGC 4258 as our geometric anchor to measure I-band (F090W vs F090W-F150W) TRGB distances to 8 hosts of 10 Type Ia supernovae (SNe Ia) within 28 Mpc: NGC 1448, NGC 1559, NGC 2525, NGC 3370, NGC 3447, NGC 5584, NGC 5643, and NGC 5861. We compare these with Hubble Space Telescope (HST) Cepheid-based relative distance moduli for the same galaxies and anchor. We find no evidence of a difference between their weighted means, 0.01 +/- 0.04 (stat) +/- 0.04 (sys) mag. We produce fourteen variants of the TRGB analysis, altering the smoothing level and color range used to measure the tips to explore their impact. For some hosts, this changes the identification of the strongest peak, but this causes little change to the sample mean difference producing a full range of 0.01 to 0.03 mag, all consistent at 1 sigma with no difference. The result matches past comparisons of I-band TRGB and Cepheids when both use HST. SNe and anchor samples observed with JWST are too small to yield a measure of H0 that is competitive with the HST sample of 42 SNe Ia and 4 anchors; however, they already provide a vital systematic crosscheck to HST measurements of the distance ladder. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.00065v3-abstract-full').style.display = 'none'; document.getElementById('2408.00065v3-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 5 figures, 4 tables, Accepted by ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 976 177 2024 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.16744">arXiv:2407.16744</a> <span> [<a href="https://arxiv.org/pdf/2407.16744">pdf</a>, <a href="https://arxiv.org/format/2407.16744">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Evaluating Cosmological Biases using Photometric Redshifts for Type Ia Supernova Cosmology with the Dark Energy Survey Supernova Program </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Myles%2C+J">J. Myles</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">H. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a> , et al. (51 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.16744v1-abstract-short" style="display: inline;"> Cosmological analyses with Type Ia Supernovae (SNe Ia) have traditionally been reliant on spectroscopy for both classifying the type of supernova and obtaining reliable redshifts to measure the distance-redshift relation. While obtaining a host-galaxy spectroscopic redshift for most SNe is feasible for small-area transient surveys, it will be too resource intensive for upcoming large-area surveys… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.16744v1-abstract-full').style.display = 'inline'; document.getElementById('2407.16744v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.16744v1-abstract-full" style="display: none;"> Cosmological analyses with Type Ia Supernovae (SNe Ia) have traditionally been reliant on spectroscopy for both classifying the type of supernova and obtaining reliable redshifts to measure the distance-redshift relation. While obtaining a host-galaxy spectroscopic redshift for most SNe is feasible for small-area transient surveys, it will be too resource intensive for upcoming large-area surveys such as the Vera Rubin Observatory Legacy Survey of Space and Time, which will observe on the order of millions of SNe. Here we use data from the Dark Energy Survey (DES) to address this problem with photometric redshifts (photo-z) inferred directly from the SN light-curve in combination with Gaussian and full p(z) priors from host-galaxy photo-z estimates. Using the DES 5-year photometrically-classified SN sample, we consider several photo-z algorithms as host-galaxy photo-z priors, including the Self-Organizing Map redshifts (SOMPZ), Bayesian Photometric Redshifts (BPZ), and Directional-Neighbourhood Fitting (DNF) redshift estimates employed in the DES 3x2 point analyses. With detailed catalog-level simulations of the DES 5-year sample, we find that the simulated w can be recovered within $\pm$0.02 when using SN+SOMPZ or DNF prior photo-z, smaller than the average statistical uncertainty for these samples of 0.03. With data, we obtain biases in w consistent with simulations within ~1$蟽$ for three of the five photo-z variants. We further evaluate how photo-z systematics interplay with photometric classification and find classification introduces a subdominant systematic component. This work lays the foundation for next-generation fully photometric SNe Ia cosmological analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.16744v1-abstract-full').style.display = 'none'; document.getElementById('2407.16744v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 9 figures. Submitting to MNRAS, comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05051">arXiv:2406.05051</a> <span> [<a href="https://arxiv.org/pdf/2406.05051">pdf</a>, <a href="https://arxiv.org/format/2406.05051">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Modelling the impact of host galaxy dust on type Ia supernova distance measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Gait%C3%A1n%2C+S">S. Gonz谩lez-Gait谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Duarte%2C+J">J. Duarte</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Carollo%2C+D">D. Carollo</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">K. Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+G+F">G. F. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Nichol%2C+R+C">R. C. Nichol</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Toy%2C+M">M. Toy</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+B+E">B. E. Tucker</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a> , et al. (43 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.05051v1-abstract-short" style="display: inline;"> Type Ia Supernovae (SNe Ia) are a critical tool in measuring the accelerating expansion of the universe. Recent efforts to improve these standard candles have focused on incorporating the effects of dust on distance measurements with SNe Ia. In this paper, we use the state-of-the-art Dark Energy Survey 5 year sample to evaluate two different families of dust models: empirical extinction models der… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05051v1-abstract-full').style.display = 'inline'; document.getElementById('2406.05051v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05051v1-abstract-full" style="display: none;"> Type Ia Supernovae (SNe Ia) are a critical tool in measuring the accelerating expansion of the universe. Recent efforts to improve these standard candles have focused on incorporating the effects of dust on distance measurements with SNe Ia. In this paper, we use the state-of-the-art Dark Energy Survey 5 year sample to evaluate two different families of dust models: empirical extinction models derived from SNe Ia data, and physical attenuation models from the spectra of galaxies. Among the SNe Ia-derived models, we find that a logistic function of the total-to-selective extinction RV best recreates the correlations between supernova distance measurements and host galaxy properties, though an additional 0.02 magnitudes of grey scatter are needed to fully explain the scatter in SNIa brightness in all cases. These empirically-derived extinction distributions are highly incompatible with the physical attenuation models from galactic spectral measurements. From these results, we conclude that SNe Ia must either preferentially select extreme ends of galactic dust distributions, or that the characterisation of dust along the SNe Ia line-of-sight is incompatible with that of galactic dust distributions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05051v1-abstract-full').style.display = 'none'; document.getElementById('2406.05051v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05050">arXiv:2406.05050</a> <span> [<a href="https://arxiv.org/pdf/2406.05050">pdf</a>, <a href="https://arxiv.org/format/2406.05050">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Survey Supernova Program: Slow supernovae show cosmological time dilation out to $z \sim 1$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=White%2C+R+M+T">R. M. T. White</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+G+F">G. F. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">K. Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Hinton%2C+S+R">S. R. Hinton</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a> , et al. (45 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.05050v2-abstract-short" style="display: inline;"> We present a precise measurement of cosmological time dilation using the light curves of 1504 type Ia supernovae from the Dark Energy Survey spanning a redshift range $0.1\lesssim z\lesssim 1.2$. We find that the width of supernova light curves is proportional to $(1+z)$, as expected for time dilation due to the expansion of the Universe. Assuming type Ia supernovae light curves are emitted with a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05050v2-abstract-full').style.display = 'inline'; document.getElementById('2406.05050v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05050v2-abstract-full" style="display: none;"> We present a precise measurement of cosmological time dilation using the light curves of 1504 type Ia supernovae from the Dark Energy Survey spanning a redshift range $0.1\lesssim z\lesssim 1.2$. We find that the width of supernova light curves is proportional to $(1+z)$, as expected for time dilation due to the expansion of the Universe. Assuming type Ia supernovae light curves are emitted with a consistent duration $螖t_{\rm em}$, and parameterising the observed duration as $螖t_{\rm obs}=螖t_{\rm em}(1+z)^b$, we fit for the form of time dilation using two methods. Firstly, we find that a power of $b \approx 1$ minimises the flux scatter in stacked subsamples of light curves across different redshifts. Secondly, we fit each target supernova to a stacked light curve (stacking all supernovae with observed bandpasses matching that of the target light curve) and find $b=1.003\pm0.005$ (stat) $\pm\,0.010$ (sys). Thanks to the large number of supernovae and large redshift-range of the sample, this analysis gives the most precise measurement of cosmological time dilation to date, ruling out any non-time-dilating cosmological models at very high significance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05050v2-abstract-full').style.display = 'none'; document.getElementById('2406.05050v2-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 13 figures. Updated in response to reviewer feedback. Accepted for publication in the Monthly Notices of the Royal Astronomical Society (MNRAS)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-24-0293-PPD, DES-2024-0831 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05049">arXiv:2406.05049</a> <span> [<a href="https://arxiv.org/pdf/2406.05049">pdf</a>, <a href="https://arxiv.org/format/2406.05049">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Survey Supernova Program: An updated measurement of the Hubble constant using the Inverse Distance Ladder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Camilleri%2C+R">R. Camilleri</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Hinton%2C+S+R">S. R. Hinton</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">K. Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Nichol%2C+R+C">R. C. Nichol</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a> , et al. (55 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.05049v1-abstract-short" style="display: inline;"> We measure the current expansion rate of the Universe, Hubble's constant $H_0$, by calibrating the absolute magnitudes of supernovae to distances measured by Baryon Acoustic Oscillations. This `inverse distance ladder' technique provides an alternative to calibrating supernovae using nearby absolute distance measurements, replacing the calibration with a high-redshift anchor. We use the recent rel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05049v1-abstract-full').style.display = 'inline'; document.getElementById('2406.05049v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05049v1-abstract-full" style="display: none;"> We measure the current expansion rate of the Universe, Hubble's constant $H_0$, by calibrating the absolute magnitudes of supernovae to distances measured by Baryon Acoustic Oscillations. This `inverse distance ladder' technique provides an alternative to calibrating supernovae using nearby absolute distance measurements, replacing the calibration with a high-redshift anchor. We use the recent release of 1829 supernovae from the Dark Energy Survey spanning $0.01\lt z \lt1.13$ anchored to the recent Baryon Acoustic Oscillation measurements from DESI spanning $0.30 \lt z_{\mathrm{eff}} \lt 2.33$. To trace cosmology to $z=0$, we use the third-, fourth- and fifth-order cosmographic models, which, by design, are agnostic about the energy content and expansion history of the universe. With the inclusion of the higher-redshift DESI-BAO data, the third-order model is a poor fit to both data sets, with the fourth-order model being preferred by the Akaike Information Criterion. Using the fourth-order cosmographic model, we find $H_0=67.19^{+0.66}_{-0.64}\mathrm{~km} \mathrm{~s}^{-1} \mathrm{~Mpc}^{-1}$, in agreement with the value found by Planck without the need to assume Flat-$螞$CDM. However the best-fitting expansion history differs from that of Planck, providing continued motivation to investigate these tensions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05049v1-abstract-full').style.display = 'none'; document.getElementById('2406.05049v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05048">arXiv:2406.05048</a> <span> [<a href="https://arxiv.org/pdf/2406.05048">pdf</a>, <a href="https://arxiv.org/format/2406.05048">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stae1988">10.1093/mnras/stae1988 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Survey Supernova Program: Investigating Beyond-$螞$CDM </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Camilleri%2C+R">R. Camilleri</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Frieman%2C+J">J. Frieman</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+A">A. Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">K. Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Hinton%2C+S+R">S. R. Hinton</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">H. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+G">G. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Toy%2C+M">M. Toy</a> , et al. (55 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.05048v2-abstract-short" style="display: inline;"> We report constraints on a variety of non-standard cosmological models using the full 5-year photometrically-classified type Ia supernova sample from the Dark Energy Survey (DES-SN5YR). Both Akaike Information Criterion (AIC) and Suspiciousness calculations find no strong evidence for or against any of the non-standard models we explore. When combined with external probes, the AIC and Suspiciousne… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05048v2-abstract-full').style.display = 'inline'; document.getElementById('2406.05048v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05048v2-abstract-full" style="display: none;"> We report constraints on a variety of non-standard cosmological models using the full 5-year photometrically-classified type Ia supernova sample from the Dark Energy Survey (DES-SN5YR). Both Akaike Information Criterion (AIC) and Suspiciousness calculations find no strong evidence for or against any of the non-standard models we explore. When combined with external probes, the AIC and Suspiciousness agree that 11 of the 15 models are moderately preferred over Flat-$螞$CDM suggesting additional flexibility in our cosmological models may be required beyond the cosmological constant. We also provide a detailed discussion of all cosmological assumptions that appear in the DES supernova cosmology analyses, evaluate their impact, and provide guidance on using the DES Hubble diagram to test non-standard models. An approximate cosmological model, used to perform bias corrections to the data holds the biggest potential for harbouring cosmological assumptions. We show that even if the approximate cosmological model is constructed with a matter density shifted by $螖惟_m\sim0.2$ from the true matter density of a simulated data set the bias that arises is sub-dominant to statistical uncertainties. Nevertheless, we present and validate a methodology to reduce this bias. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05048v2-abstract-full').style.display = 'none'; document.getElementById('2406.05048v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published to MNRAS on 20 August 2024; v2 updates to the accepted version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-24-0291-PPD </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05047">arXiv:2406.05047</a> <span> [<a href="https://arxiv.org/pdf/2406.05047">pdf</a>, <a href="https://arxiv.org/format/2406.05047">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Survey : Detection of weak lensing magnification of supernovae and constraints on dark matter haloes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Frieman%2C+J">J. Frieman</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Lahav%2C+O">O. Lahav</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Nichol%2C+R+C">R. C. Nichol</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Annis%2C+J">J. Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a> , et al. (40 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.05047v1-abstract-short" style="display: inline;"> The residuals of the distance moduli of Type Ia supernovae (SN Ia) relative to a Hubble diagram fit contain information about the inhomogeneity of the universe, due to weak lensing magnification by foreground matter. By correlating the residuals of the Dark Energy Survey Year 5 SN Ia sample (DES-SN5YR) with extra-galactic foregrounds from the DES Y3 Gold catalog, we detect the presence of lensing… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05047v1-abstract-full').style.display = 'inline'; document.getElementById('2406.05047v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05047v1-abstract-full" style="display: none;"> The residuals of the distance moduli of Type Ia supernovae (SN Ia) relative to a Hubble diagram fit contain information about the inhomogeneity of the universe, due to weak lensing magnification by foreground matter. By correlating the residuals of the Dark Energy Survey Year 5 SN Ia sample (DES-SN5YR) with extra-galactic foregrounds from the DES Y3 Gold catalog, we detect the presence of lensing at $6.0 蟽$ significance. This is the first detection with a significance level above $5蟽$. Constraints on the effective mass-to-light ratios and radial profiles of dark-matter haloes surrounding individual galaxies are also obtained. We show that the scatter of SNe Ia around the Hubble diagram is reduced by modifying the standardisation of the distance moduli to include an easily calculable de-lensing (i.e., environmental) term. We use the de-lensed distance moduli to recompute cosmological parameters derived from SN Ia, finding in Flat $w$CDM a difference of $螖惟_{\rm M} = +0.036$ and $螖w = -0.056$ compared to the unmodified distance moduli, a change of $\sim 0.3蟽$. We argue that our modelling of SN Ia lensing will lower systematics on future surveys with higher statistical power. We use the observed dispersion of lensing in DES-SN5YR to constrain $蟽_8$, but caution that the fit is sensitive to uncertainties at small scales. Nevertheless, our detection of SN Ia lensing opens a new pathway to study matter inhomogeneity that complements galaxy-galaxy lensing surveys and has unrelated systematics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05047v1-abstract-full').style.display = 'none'; document.getElementById('2406.05047v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05046">arXiv:2406.05046</a> <span> [<a href="https://arxiv.org/pdf/2406.05046">pdf</a>, <a href="https://arxiv.org/format/2406.05046">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Survey Supernova Program: Light curves and 5-Year data release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Herner%2C+K">K. Herner</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Acevedo%2C+M">M. Acevedo</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">H. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Rose%2C+B">B. Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Camilleri%2C+R">R. Camilleri</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Kovacs%2C+E">E. Kovacs</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Toy%2C+M">M. Toy</a> , et al. (60 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.05046v1-abstract-short" style="display: inline;"> We present $griz$ photometric light curves for the full 5 years of the Dark Energy Survey Supernova program (DES-SN), obtained with both forced Point Spread Function (PSF) photometry on Difference Images (DIFFIMG) performed during survey operations, and Scene Modelling Photometry (SMP) on search images processed after the survey. This release contains $31,636$ DIFFIMG and $19,706$ high-quality SMP… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05046v1-abstract-full').style.display = 'inline'; document.getElementById('2406.05046v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05046v1-abstract-full" style="display: none;"> We present $griz$ photometric light curves for the full 5 years of the Dark Energy Survey Supernova program (DES-SN), obtained with both forced Point Spread Function (PSF) photometry on Difference Images (DIFFIMG) performed during survey operations, and Scene Modelling Photometry (SMP) on search images processed after the survey. This release contains $31,636$ DIFFIMG and $19,706$ high-quality SMP light curves, the latter of which contains $1635$ photometrically-classified supernovae that pass cosmology quality cuts. This sample spans the largest redshift ($z$) range ever covered by a single SN survey ($0.1<z<1.13$) and is the largest single sample from a single instrument of SNe ever used for cosmological constraints. We describe in detail the improvements made to obtain the final DES-SN photometry and provide a comparison to what was used in the DES-SN3YR spectroscopically-confirmed SN Ia sample. We also include a comparative analysis of the performance of the SMP photometry with respect to the real-time DIFFIMG forced photometry and find that SMP photometry is more precise, more accurate, and less sensitive to the host-galaxy surface brightness anomaly. The public release of the light curves and ancillary data can be found at https://github.com/des-science/DES-SN5YR. Finally, we discuss implications for future transient surveys, such as the forthcoming Vera Rubin Observatory Legacy Survey of Space and Time (LSST). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05046v1-abstract-full').style.display = 'none'; document.getElementById('2406.05046v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.08038">arXiv:2404.08038</a> <span> [<a href="https://arxiv.org/pdf/2404.08038">pdf</a>, <a href="https://arxiv.org/format/2404.08038">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad630e">10.3847/1538-4357/ad630e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Small Magellanic Cloud Cepheids Observed with the Hubble Space Telescope Provide a New Anchor for the SH0ES Distance Ladder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Breuval%2C+L">Louise Breuval</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=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Wenlong Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Macri%2C+L+M">Lucas M. Macri</a>, <a href="/search/astro-ph?searchtype=author&query=Romaniello%2C+M">Martino Romaniello</a>, <a href="/search/astro-ph?searchtype=author&query=Murakami%2C+Y+S">Yukei S. Murakami</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">Igor Soszy艅ski</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.08038v2-abstract-short" style="display: inline;"> We present phase-corrected photometric measurements of 88 Cepheid variables in the core of the Small Magellanic Cloud (SMC), the first sample obtained with the Hubble Space Telescope's (HST) Wide Field Camera 3, in the same homogeneous photometric system as past measurements of all Cepheids on the SH0ES distance ladder. We limit the sample to the inner core and model the geometry to reduce errors… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.08038v2-abstract-full').style.display = 'inline'; document.getElementById('2404.08038v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.08038v2-abstract-full" style="display: none;"> We present phase-corrected photometric measurements of 88 Cepheid variables in the core of the Small Magellanic Cloud (SMC), the first sample obtained with the Hubble Space Telescope's (HST) Wide Field Camera 3, in the same homogeneous photometric system as past measurements of all Cepheids on the SH0ES distance ladder. We limit the sample to the inner core and model the geometry to reduce errors in prior studies due to the nontrivial depth of this cloud. Without crowding present in ground-based studies, we obtain an unprecedentedly low dispersion of 0.102 mag for a period-luminosity (P-L) relation in the SMC, approaching the width of the Cepheid instability strip. The new geometric distance to 15 late-type detached eclipsing binaries in the SMC offers a rare opportunity to improve the foundation of the distance ladder, increasing the number of calibrating galaxies from three to four. With the SMC as the only anchor, we find H$_0\!=\!74.1 \pm 2.1$ km/s/Mpc. Combining these four geometric distances with our HST photometry of SMC Cepheids, we obtain H$_0\!=\!73.17 \pm 0.86$ km/s/Mpc. By including the SMC in the distance ladder, we also double the range where the metallicity ([Fe/H]) dependence of the Cepheid P-L relation can be calibrated, and we find $纬= -0.234 \pm 0.052$ mag/dex. Our local measurement of H$_0$ based on Cepheids and Type Ia supernovae shows a 5.8$蟽$ tension with the value inferred from the cosmic microwave background assuming a Lambda cold dark matter ($螞$CDM) cosmology, reinforcing the possibility of physics beyond $螞$CDM. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.08038v2-abstract-full').style.display = 'none'; document.getElementById('2404.08038v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ. Data Tables are available at: https://github.com/lbreuval/SMC_Cepheids_HST</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal (2024), 973, 30 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.13885">arXiv:2403.13885</a> <span> [<a href="https://arxiv.org/pdf/2403.13885">pdf</a>, <a href="https://arxiv.org/format/2403.13885">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/10.1051/0004-6361/202450052">10.1051/0004-6361/202450052 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The DEHVILS in the Details: Type Ia Supernova Hubble Residual Comparisons and Mass Step Analysis in the Near-Infrared </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+E+R">Erik R. Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+O">David O. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Do%2C+A">Aaron Do</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">Brodie Popovic</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=Dwomoh%2C+A">Arianna Dwomoh</a>, <a href="/search/astro-ph?searchtype=author&query=Johansson%2C+J">Joel Johansson</a>, <a href="/search/astro-ph?searchtype=author&query=Rubin%2C+D">David Rubin</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">Bruno O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">Benjamin J. Shappee</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=Tully%2C+R+B">R. Brent Tully</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">Maria Vincenzi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.13885v2-abstract-short" style="display: inline;"> Measurements of Type Ia Supernovae (SNe Ia) in the near-infrared (NIR) have been used both as an alternate path to cosmology compared to optical measurements and as a method of constraining key systematics for the larger optical studies. With the DEHVILS sample, the largest published NIR sample with consistent NIR coverage of maximum light across three NIR bands ($Y$, $J$, and $H$), we check three… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13885v2-abstract-full').style.display = 'inline'; document.getElementById('2403.13885v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.13885v2-abstract-full" style="display: none;"> Measurements of Type Ia Supernovae (SNe Ia) in the near-infrared (NIR) have been used both as an alternate path to cosmology compared to optical measurements and as a method of constraining key systematics for the larger optical studies. With the DEHVILS sample, the largest published NIR sample with consistent NIR coverage of maximum light across three NIR bands ($Y$, $J$, and $H$), we check three key systematics: (i) the reduction in Hubble residual scatter as compared to the optical, (ii) the measurement of a "mass step" or lack thereof and its implications, and (iii) the ability to distinguish between various dust models by analyzing slopes and correlations between Hubble residuals in the NIR and optical. We produce SN Ia simulations of the DEHVILS sample and find that it is $\textit{harder}$ to differentiate between various dust models than previously understood. Additionally, we find that fitting with the current SALT3-NIR model does not yield accurate wavelength-dependent stretch-luminosity correlations, and we propose a limited solution for this problem. From the data, we see that (i) the standard deviation of Hubble residual values from NIR bands treated as standard candles are 0.007-0.042 mag smaller than those in the optical, (ii) the NIR mass step is not constrainable with the current sample size of 47 SNe Ia from DEHVILS, and (iii) Hubble residuals in the NIR and optical are correlated in the data. We test a few variations on the number and combinations of filters and data samples, and we observe that none of our findings or conclusions are significantly impacted by these modifications. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13885v2-abstract-full').style.display = 'none'; document.getElementById('2403.13885v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 10 figures. Accepted by A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A56 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.05620">arXiv:2403.05620</a> <span> [<a href="https://arxiv.org/pdf/2403.05620">pdf</a>, <a href="https://arxiv.org/format/2403.05620">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stae2501">10.1093/mnras/stae2501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hawai'i Supernova Flows: A Peculiar Velocity Survey Using Over a Thousand Supernovae in the Near-Infrared </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Do%2C+A">Aaron Do</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">Benjamin J. Shappee</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=Tully%2C+R+B">R. Brent Tully</a>, <a href="/search/astro-ph?searchtype=author&query=de+Jaeger%2C+T">Thomas de Jaeger</a>, <a href="/search/astro-ph?searchtype=author&query=Rubin%2C+D">David Rubin</a>, <a href="/search/astro-ph?searchtype=author&query=Ashall%2C+C">Chris Ashall</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+C+R">Christopher R. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+D+D">Dhvanil D. Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Hinkle%2C+J+T">Jason T. Hinkle</a>, <a href="/search/astro-ph?searchtype=author&query=Hoogendam%2C+W+B">Willem B. Hoogendam</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+M+E">Mark E. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+O">David O. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Mandel%2C+K+S">Kaisey S. Mandel</a>, <a href="/search/astro-ph?searchtype=author&query=Payne%2C+A+V">Anna V. Payne</a>, <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+E+R">Erik R. Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+M+A">Michael A. Tucker</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.05620v2-abstract-short" style="display: inline;"> We introduce the Hawai'i Supernova Flows project and present summary statistics of the first 1,217 astronomical transients observed, 668 of which are spectroscopically classified Type Ia Supernovae (SNe Ia). Our project is designed to obtain systematics-limited distances to SNe Ia while consuming minimal dedicated observational resources. To date, we have performed almost 5,000 near-infrared (NIR)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.05620v2-abstract-full').style.display = 'inline'; document.getElementById('2403.05620v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.05620v2-abstract-full" style="display: none;"> We introduce the Hawai'i Supernova Flows project and present summary statistics of the first 1,217 astronomical transients observed, 668 of which are spectroscopically classified Type Ia Supernovae (SNe Ia). Our project is designed to obtain systematics-limited distances to SNe Ia while consuming minimal dedicated observational resources. To date, we have performed almost 5,000 near-infrared (NIR) observations of astronomical transients and have obtained spectra for over 200 host galaxies lacking published spectroscopic redshifts. In this survey paper we describe the methodology used to select targets, collect/reduce data, calculate distances, and perform quality cuts. We compare our methods to those used in similar studies, finding general agreement or mild improvement. Our summary statistics include various parametrizations of dispersion in the Hubble diagrams produced using fits to several commonly used SN Ia models. We find the lowest dispersions using the \texttt{SNooPy} package's EBV\_model2, with a root mean square (RMS) deviation of 0.165 mag and a normalized median absolute deviation (NMAD) of 0.123 mag. The full utility of the Hawai'i Supernova Flows data set far exceeds the analyses presented in this paper. Our photometry will provide a valuable test bed for models of SN Ia incorporating NIR data. Differential cosmological studies comparing optical samples and combined optical and NIR samples will have increased leverage for constraining chromatic effects like dust extinction. We invite the community to explore our data by making the light curves, fits, and host galaxy redshifts publicly accessible. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.05620v2-abstract-full').style.display = 'none'; document.getElementById('2403.05620v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS. 43 pages, 26 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/2402.13484">arXiv:2402.13484</a> <span> [<a href="https://arxiv.org/pdf/2402.13484">pdf</a>, <a href="https://arxiv.org/format/2402.13484">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/10.1017/pasa.2024.74">10.1017/pasa.2024.74 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> WiFeS observations of nearby southern Type Ia supernova host galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carr%2C+A">Anthony Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">Tamara M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Camilleri%2C+R">Ryan Camilleri</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">Chris Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Freeman%2C+K+C">Kenneth C. Freeman</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.13484v2-abstract-short" style="display: inline;"> We present high-resolution observations of nearby ($z\lesssim 0.1$) galaxies that have hosted Type Ia supernovae to measure systemic spectroscopic redshifts using the Wide Field Spectrograph (WiFeS) instrument on the Australian National University 2.3 m telescope at Siding Spring Observatory. While most of the galaxies targeted have previous spectroscopic redshifts, we provide demonstrably more ac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.13484v2-abstract-full').style.display = 'inline'; document.getElementById('2402.13484v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.13484v2-abstract-full" style="display: none;"> We present high-resolution observations of nearby ($z\lesssim 0.1$) galaxies that have hosted Type Ia supernovae to measure systemic spectroscopic redshifts using the Wide Field Spectrograph (WiFeS) instrument on the Australian National University 2.3 m telescope at Siding Spring Observatory. While most of the galaxies targeted have previous spectroscopic redshifts, we provide demonstrably more accurate and precise redshifts with competitive uncertainties, motivated by potential systematic errors that could bias estimates of the Hubble constant ($H_0$). The WiFeS instrument is remarkably stable; after calibration, the wavelength solution varies by $\lesssim 0.5$ 脜 in red and blue with no evidence of a trend over the course of several years. By virtue of the $25\times 38$ arcsec field of view, we are always able to redshift the galactic core, or the entire galaxy in the cases where its angular extent is smaller than the field of view, reducing any errors due to galaxy rotation. We observed 185 southern SN Ia host galaxies and redshifted each via at least one spatial region of a) the core, and b) the average over the full-field/entire galaxy. Overall, we find stochastic differences between historical redshifts and our measured redshifts on the order of $\lesssim 10^{-3}$ with a mean offset of $4.3\times 10^{-5}$, and normalised median absolute deviation of $1.2\times 10^{-4}$. We show that a systematic redshift offset at this level is not enough to bias cosmology, as $H_0$ shifts by $+0.1$ km s$^{-1}$ Mpc$^{-1}$ when we replace Pantheon+ redshifts with our own, but the occasional large differences are interesting to note. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.13484v2-abstract-full').style.display = 'none'; document.getElementById('2402.13484v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 16 figures, 3 tables. Accepted for publication in PASA. Added Zenodo data link</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Publ. Astron. Soc. Aust. 41 (2024) e068 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.04777">arXiv:2401.04777</a> <span> [<a href="https://arxiv.org/pdf/2401.04777">pdf</a>, <a href="https://arxiv.org/format/2401.04777">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad2f2b">10.3847/1538-4357/ad2f2b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Reconnaissance with JWST of the J-region Asymptotic Giant Branch in Distance Ladder Galaxies: From Irregular Luminosity Functions to Approximation of the Hubble Constant </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+S">Siyang Li</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=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D+M">Daniel M. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Wenlong Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Breuval%2C+L">Louise Breuval</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+C+D">Caroline D. Huang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.04777v2-abstract-short" style="display: inline;"> We study stars in the J-regions of the asymptotic giant branch (JAGB) of near-infrared color magnitude diagrams in the maser host NGC 4258 and 4 hosts of 6 Type Ia supernovae (SN Ia): NGC 1448, NGC 1559, NGC 5584, and NGC 5643. These clumps of stars are readily apparent near $1.0<F150W-F277W<1.5$ and $m_{F150W}$=22-25 mag with James Webb Space Telescope NIRCam photometry. Various methods have been… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04777v2-abstract-full').style.display = 'inline'; document.getElementById('2401.04777v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.04777v2-abstract-full" style="display: none;"> We study stars in the J-regions of the asymptotic giant branch (JAGB) of near-infrared color magnitude diagrams in the maser host NGC 4258 and 4 hosts of 6 Type Ia supernovae (SN Ia): NGC 1448, NGC 1559, NGC 5584, and NGC 5643. These clumps of stars are readily apparent near $1.0<F150W-F277W<1.5$ and $m_{F150W}$=22-25 mag with James Webb Space Telescope NIRCam photometry. Various methods have been proposed to assign an apparent reference magnitude for this recently proposed standard candle, including the mode, median, sigma-clipped mean or a modeled luminosity function parameter. We test the consistency of these by measuring intra-host variations, finding differences of up to $\sim$0.2 mag that significantly exceed statistical uncertainties. Brightness differences appear intrinsic, and are further amplified by the non-uniform shape of the JAGB luminosity function, also apparent in the LMC and SMC. We follow a 'many methods' approach to consistently measure JAGB magnitudes and distances to the SN Ia host sample calibrated by NGC 4258. We find broad agreement with distances measured from Cepheids, tip of the red giant branch (TRGB), and Miras. However, the SN host mean distance estimated via the JAGB method necessary to estimate $H_0$ differs by $\sim$0.19 mag amongst the above definitions, a result of different levels of luminosity function asymmetry. The methods yield a full range of $71-78$ km s$^{-1}$ Mpc$^{-1}$, i.e., a fiducial result of $H_0=74.7\pm2.1$ (stat) $\pm$2.3 (sys) ($\pm$3.1 if combined in quadrature) km s$^{-1}$ Mpc$^{-1}$, with systematic errors limited by the differences in methods. Future work may seek to further standardize and refine this promising tool, making it more competitive with established distance indicators. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04777v2-abstract-full').style.display = 'none'; document.getElementById('2401.04777v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 21 figures, 8 tables, Accepted by ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 966 20 2024 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.04776">arXiv:2401.04776</a> <span> [<a href="https://arxiv.org/pdf/2401.04776">pdf</a>, <a href="https://arxiv.org/format/2401.04776">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Tip of the Red Giant Branch Distances with JWST: An Absolute Calibration in NGC 4258 and First Applications to Type Ia Supernova Hosts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</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=Yuan%2C+W">Wenlong Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachael Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+S">Siyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Makarov%2C+D+I">Dmitry I. Makarov</a>, <a href="/search/astro-ph?searchtype=author&query=Makarova%2C+L+N">Lidia N. Makarova</a>, <a href="/search/astro-ph?searchtype=author&query=Tully%2C+R+B">R. Brent Tully</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Breuval%2C+L">Louise Breuval</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Karachentsev%2C+I+D">Igor D. Karachentsev</a>, <a href="/search/astro-ph?searchtype=author&query=Macri%2C+L+M">Lucas M. Macri</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.04776v2-abstract-short" style="display: inline;"> The tip of the red giant branch (TRGB) allows for the measurement of precise and accurate distances to nearby galaxies, based on the brightest ascent of low-mass red giant branch stars before they undergo the helium flash. With the advent of JWST, there is great promise to utilize the technique to measure galaxy distances out to at least 50 Mpc, significantly further than HST's reach of 20 Mpc. Ho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04776v2-abstract-full').style.display = 'inline'; document.getElementById('2401.04776v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.04776v2-abstract-full" style="display: none;"> The tip of the red giant branch (TRGB) allows for the measurement of precise and accurate distances to nearby galaxies, based on the brightest ascent of low-mass red giant branch stars before they undergo the helium flash. With the advent of JWST, there is great promise to utilize the technique to measure galaxy distances out to at least 50 Mpc, significantly further than HST's reach of 20 Mpc. However, with any standard candle, it is first necessary to provide an absolute reference. Here we use Cycle 1 data to provide an absolute calibration in the F090W filter. F090W is most similar to the F814W filter commonly used for TRGB measurements with HST, which had been adopted by the community due to minimal dependence from the underlying metallicities and ages of stars. The imaging we use was taken in the outskirts of NGC 4258, which has a direct geometrical distance measurement from the Keplerian motion of its water megamaser. Utilizing several measurement techniques, we find $M_{TRGB}^{F090W}$ = -4.362 $\pm$ 0.033 (stat) $\pm$ 0.045 (sys) mag (Vega) for the metal-poor TRGB. We also perform measurements of the TRGB in two Type Ia supernova hosts, NGC 1559, and NGC 5584. We find good agreement between our TRGB distances and previous distance determinations to these galaxies from Cepheids ($螖$ = 0.01 $\pm$ 0.06 mag), with these differences being too small to explain the Hubble tension ($\sim$0.17 mag). As a final bonus, we showcase the serendipitous discovery of a faint dwarf galaxy near NGC 5584. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04776v2-abstract-full').style.display = 'none'; document.getElementById('2401.04776v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 12 figures, accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.04773">arXiv:2401.04773</a> <span> [<a href="https://arxiv.org/pdf/2401.04773">pdf</a>, <a href="https://arxiv.org/format/2401.04773">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> JWST Observations Reject Unrecognized Crowding of Cepheid Photometry as an Explanation for the Hubble Tension at 8 sigma Confidence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Wenlong Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Macri%2C+L+M">Lucas M. Macri</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Breuval%2C+L">Louise Breuval</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Perrin%2C+M">Marshall Perrin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.04773v1-abstract-short" style="display: inline;"> We present high-definition observations with the James Webb Space Telescope of >1000 Cepheids in a geometric anchor of the distance ladder, NGC4258, and in 5 hosts of 8 SNe~Ia, a far greater sample than previous studies with JWST. These galaxies individually contain the largest samples of Cepheids, an average of >150 each, producing the strongest statistical comparison to those previously measured… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04773v1-abstract-full').style.display = 'inline'; document.getElementById('2401.04773v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.04773v1-abstract-full" style="display: none;"> We present high-definition observations with the James Webb Space Telescope of >1000 Cepheids in a geometric anchor of the distance ladder, NGC4258, and in 5 hosts of 8 SNe~Ia, a far greater sample than previous studies with JWST. These galaxies individually contain the largest samples of Cepheids, an average of >150 each, producing the strongest statistical comparison to those previously measured with the Hubble Space Telescope in the NIR. They also span the distance range of those used to determine the Hubble constant with HST, allowing us to search for a distance-dependent bias in HST measurements. The superior resolution of JWST negates crowding noise, the largest source of variance in the NIR Cepheid Period-Luminosity relations (Leavitt laws) measured with HST. Together with the use of two-epochs to constrain Cepheid phases and three filters to remove reddening, we reduce the dispersion in the Cepheid PL relations by a factor of 2.5. We find no significant difference in the mean distance measurements determined from HST and JWST, with a formal difference of -0.01+/-0.03 mag. This result is independent of zeropoints and analysis variants including metallicity dependence, local crowding, choice of filters, and relation slope. We can reject the hypothesis of unrecognized crowding of Cepheid photometry from HST that grows with distance as the cause of the ``Hubble Tension'' at 8.2 sigma, i.e., greater confidence than that of the Hubble Tension itself. We conclude that errors in photometric measurements of Cepheids across the distance ladder do not significantly contribute to the Tension. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04773v1-abstract-full').style.display = 'none'; document.getElementById('2401.04773v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ Letters, accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.02945">arXiv:2401.02945</a> <span> [<a href="https://arxiv.org/pdf/2401.02945">pdf</a>, <a href="https://arxiv.org/format/2401.02945">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+G">G. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Acevedo%2C+M">M. Acevedo</a>, <a href="/search/astro-ph?searchtype=author&query=Camilleri%2C+R">R. Camilleri</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Hinton%2C+S+R">S. R. Hinton</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">H. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+B">B. Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Bassett%2C+B+A">B. A. Bassett</a>, <a href="/search/astro-ph?searchtype=author&query=Carollo%2C+D">D. Carollo</a> , et al. (71 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="2401.02945v2-abstract-short" style="display: inline;"> We present the full Hubble diagram of photometrically-classified Type Ia supernovae (SNe Ia) from the Dark Energy Survey supernova program (DES-SN). DES-SN discovered more than 20,000 SN candidates and obtained spectroscopic redshifts of 7,000 host galaxies. Based on the light-curve quality, we select 1635 photometrically-identified SNe Ia with spectroscopic redshift 0.10$< z <$1.13, which is the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02945v2-abstract-full').style.display = 'inline'; document.getElementById('2401.02945v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.02945v2-abstract-full" style="display: none;"> We present the full Hubble diagram of photometrically-classified Type Ia supernovae (SNe Ia) from the Dark Energy Survey supernova program (DES-SN). DES-SN discovered more than 20,000 SN candidates and obtained spectroscopic redshifts of 7,000 host galaxies. Based on the light-curve quality, we select 1635 photometrically-identified SNe Ia with spectroscopic redshift 0.10$< z <$1.13, which is the largest sample of supernovae from any single survey and increases the number of known $z>0.5$ supernovae by a factor of five. In a companion paper, we present cosmological results of the DES-SN sample combined with 194 spectroscopically-classified SNe Ia at low redshift as an anchor for cosmological fits. Here we present extensive modeling of this combined sample and validate the entire analysis pipeline used to derive distances. We show that the statistical and systematic uncertainties on cosmological parameters are $蟽_{惟_M,{\rm stat+sys}}^{螞{\rm CDM}}=$0.017 in a flat $螞$CDM model, and $(蟽_{惟_M},蟽_w)_{\rm stat+sys}^{w{\rm CDM}}=$(0.082, 0.152) in a flat $w$CDM model. Combining the DES SN data with the highly complementary CMB measurements by Planck Collaboration (2020) reduces uncertainties on cosmological parameters by a factor of 4. In all cases, statistical uncertainties dominate over systematics. We show that uncertainties due to photometric classification make up less than 10% of the total systematic uncertainty budget. This result sets the stage for the next generation of SN cosmology surveys such as the Vera C. Rubin Observatory's Legacy Survey of Space and Time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02945v2-abstract-full').style.display = 'none'; document.getElementById('2401.02945v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">39 pages, 19 figures; Submitted to ApJ; companion paper Dark Energy Collaboration et al. on consecutive arxiv number 2401.02929</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-23-693-PPD </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.02929">arXiv:2401.02929</a> <span> [<a href="https://arxiv.org/pdf/2401.02929">pdf</a>, <a href="https://arxiv.org/format/2401.02929">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Survey: Cosmology Results With ~1500 New High-redshift Type Ia Supernovae Using The Full 5-year Dataset </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DES+Collaboration"> DES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Acevedo%2C+M">M. Acevedo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Amon%2C+A">A. Amon</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Annis%2C+J">J. Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bassett%2C+B+A">B. A. Bassett</a>, <a href="/search/astro-ph?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardinelli%2C+P+H">P. H. Bernardinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bernstein%2C+G+M">G. M. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Blazek%2C+J">J. Blazek</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley-Geer%2C+E">E. Buckley-Geer</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</a> , et al. (134 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="2401.02929v3-abstract-short" style="display: inline;"> We present cosmological constraints from the sample of Type Ia supernovae (SN Ia) discovered during the full five years of the Dark Energy Survey (DES) Supernova Program. In contrast to most previous cosmological samples, in which SN are classified based on their spectra, we classify the DES SNe using a machine learning algorithm applied to their light curves in four photometric bands. Spectroscop… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02929v3-abstract-full').style.display = 'inline'; document.getElementById('2401.02929v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.02929v3-abstract-full" style="display: none;"> We present cosmological constraints from the sample of Type Ia supernovae (SN Ia) discovered during the full five years of the Dark Energy Survey (DES) Supernova Program. In contrast to most previous cosmological samples, in which SN are classified based on their spectra, we classify the DES SNe using a machine learning algorithm applied to their light curves in four photometric bands. Spectroscopic redshifts are acquired from a dedicated follow-up survey of the host galaxies. After accounting for the likelihood of each SN being a SN Ia, we find 1635 DES SNe in the redshift range $0.10<z<1.13$ that pass quality selection criteria sufficient to constrain cosmological parameters. This quintuples the number of high-quality $z>0.5$ SNe compared to the previous leading compilation of Pantheon+, and results in the tightest cosmological constraints achieved by any SN data set to date. To derive cosmological constraints we combine the DES supernova data with a high-quality external low-redshift sample consisting of 194 SNe Ia spanning $0.025<z<0.10$. Using SN data alone and including systematic uncertainties we find $惟_{\rm M}=0.352\pm 0.017$ in flat $螞$CDM. Supernova data alone now require acceleration ($q_0<0$ in $螞$CDM) with over $5蟽$ confidence. We find $(惟_{\rm M},w)=(0.264^{+0.074}_{-0.096},-0.80^{+0.14}_{-0.16})$ in flat $w$CDM. For flat $w_0w_a$CDM, we find $(惟_{\rm M},w_0,w_a)=(0.495^{+0.033}_{-0.043},-0.36^{+0.36}_{-0.30},-8.8^{+3.7}_{-4.5})$. Including Planck CMB data, SDSS BAO data, and DES $3\times2$-point data gives $(惟_{\rm M},w)=(0.321\pm0.007,-0.941\pm0.026)$. In all cases dark energy is consistent with a cosmological constant to within $\sim2蟽$. In our analysis, systematic errors on cosmological parameters are subdominant compared to statistical errors; paving the way for future photometrically classified supernova analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02929v3-abstract-full').style.display = 'none'; document.getElementById('2401.02929v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 12 figures; Accepted by ApJL 29 March 2024; v3 updates to accepted version and includes links to data</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-23-0821-PPD </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.16830">arXiv:2311.16830</a> <span> [<a href="https://arxiv.org/pdf/2311.16830">pdf</a>, <a href="https://arxiv.org/format/2311.16830">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Role of Type Ia Supernovae in Constraining the Hubble Constant </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">Maria Vincenzi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.16830v1-abstract-short" style="display: inline;"> In the conventional / most studied local distance ladder measurements, Type Ia supernovae (SNe Ia) are used in two of the three rungs. In the second rung, their luminosities are calibrated by standard candles like Cepheids or Tip of the Red Giant Branch (TRGB). In the third rung, the high luminosities and standardizability allow SNe to be used to calibrate the `Hubble' relation between distances a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.16830v1-abstract-full').style.display = 'inline'; document.getElementById('2311.16830v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.16830v1-abstract-full" style="display: none;"> In the conventional / most studied local distance ladder measurements, Type Ia supernovae (SNe Ia) are used in two of the three rungs. In the second rung, their luminosities are calibrated by standard candles like Cepheids or Tip of the Red Giant Branch (TRGB). In the third rung, the high luminosities and standardizability allow SNe to be used to calibrate the `Hubble' relation between distances and redshifts. Locally, the majority of distance ladder analyses find a high value of the Hubble Constant $H_0$ of $>70$ km/s/Mpc. Given the discrepancy with the inferred value using CMB observations, great scrutiny must be given to the role supernovae play in measuring $H_0$. Here, we review the main methodology, the many crosschecks for the supernova component of the distance ladder, and the various systematics studied. We review the important role supernovae play to explain the small disagreements seen from various local analyses. We also discuss analyses that employ an inverse distance ladder, which use similar sets of supernovae, but in the reverse direction, and yield a low value of $H_0$. We conclude given all available evidence, it is difficult to find a way that a systematic in supernovae measurements, or a non-$螞$CDM component of the universe which could be measured with supernovae, can help explain the Hubble tension. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.16830v1-abstract-full').style.display = 'none'; document.getElementById('2311.16830v1-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.06178">arXiv:2311.06178</a> <span> [<a href="https://arxiv.org/pdf/2311.06178">pdf</a>, <a href="https://arxiv.org/format/2311.06178">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Evaluating the Consistency of Cosmological Distances Using Supernova Siblings in the Near-Infrared </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dwomoh%2C+A+M">Arianna M. Dwomoh</a>, <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+E+R">Erik R. Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Ashall%2C+C">Chris Ashall</a>, <a href="/search/astro-ph?searchtype=author&query=DerKacy%2C+J+M">James M. DerKacy</a>, <a href="/search/astro-ph?searchtype=author&query=Do%2C+A">Aaron Do</a>, <a href="/search/astro-ph?searchtype=author&query=Johansson%2C+J">Joel Johansson</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+O">David O. Jones</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=Shappee%2C+B+J">Benjamin J. Shappee</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.06178v2-abstract-short" style="display: inline;"> The study of supernova siblings, supernovae with the same host galaxy, is an important avenue for understanding and measuring the properties of Type Ia Supernova (SN Ia) light curves (LCs). Thus far, sibling analyses have mainly focused on optical LC data. Considering that LCs in the near-infrared (NIR) are expected to be better standard candles than those in the optical, we carry out the first an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.06178v2-abstract-full').style.display = 'inline'; document.getElementById('2311.06178v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.06178v2-abstract-full" style="display: none;"> The study of supernova siblings, supernovae with the same host galaxy, is an important avenue for understanding and measuring the properties of Type Ia Supernova (SN Ia) light curves (LCs). Thus far, sibling analyses have mainly focused on optical LC data. Considering that LCs in the near-infrared (NIR) are expected to be better standard candles than those in the optical, we carry out the first analysis compiling SN siblings with only NIR data. We perform an extensive literature search of all SN siblings and find six sets of siblings with published NIR photometry. We calibrate each set of siblings ensuring they are on homogeneous photometric systems, fit the LCs with the SALT3-NIR and SNooPy models, and find median absolute differences in $渭$ values between siblings of 0.248 mag and 0.186 mag, respectively. To evaluate the significance of these differences beyond measurement noise, we run simulations that mimic these LCs and provide an estimate for uncertainty on these median absolute differences of $\sim$0.052 mag, and we find that our analysis supports the existence of intrinsic scatter in the NIR at the 99% level. When comparing the same sets of SN siblings, we observe a median absolute difference in $渭$ values between siblings of 0.177 mag when using optical data alone as compared to 0.186 mag when using NIR data alone. We attribute this to either limited statistics, poor quality NIR data, or poor reduction of the NIR data; all of which will be improved with the Nancy Grace Roman Space Telescope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.06178v2-abstract-full').style.display = 'none'; document.getElementById('2311.06178v2-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 6 figures. Accepted into 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/2309.05654">arXiv:2309.05654</a> <span> [<a href="https://arxiv.org/pdf/2309.05654">pdf</a>, <a href="https://arxiv.org/format/2309.05654">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Amalgame: Cosmological Constraints from the First Combined Photometric Supernova Sample </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">Brodie Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">Maria Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">Mark Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">Dillon Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+B+O">Bruno O. Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">Rebecca Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+U">Utsav Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+E+R">Erik R. Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">Richard Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">Lisa Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+A+C">Ava Claire Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">Phil Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Toy%2C+M">Marcus Toy</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.05654v1-abstract-short" style="display: inline;"> Future constraints of cosmological parameters from Type Ia supernovae (SNe Ia) will depend on the use of photometric samples, those samples without spectroscopic measurements of the SNe Ia. There is a growing number of analyses that show that photometric samples can be utilised for precision cosmological studies with minimal systematic uncertainties. To investigate this claim, we perform the first… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.05654v1-abstract-full').style.display = 'inline'; document.getElementById('2309.05654v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.05654v1-abstract-full" style="display: none;"> Future constraints of cosmological parameters from Type Ia supernovae (SNe Ia) will depend on the use of photometric samples, those samples without spectroscopic measurements of the SNe Ia. There is a growing number of analyses that show that photometric samples can be utilised for precision cosmological studies with minimal systematic uncertainties. To investigate this claim, we perform the first analysis that combines two separate photometric samples, SDSS and Pan-STARRS, without including a low-redshift anchor. We evaluate the consistency of the cosmological parameters from these two samples and find they are consistent with each other to under $1蟽$. From the combined sample, named Amalgame, we measure $惟_M = 0.328 \pm 0.024$ with SN alone in a flat $螞$CDM model, and $惟_M = 0.330 \pm 0.018$ and $w = -1.016^{+0.055}_{-0.058}$ when combining with a Planck data prior and a flat $w$CDM model. These results are consistent with constraints from the Pantheon+ analysis of only spectroscopically confirmed SNe Ia, and show that there are no significant impediments to analyses of purely photometric samples of SNe Ia. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.05654v1-abstract-full').style.display = 'none'; document.getElementById('2309.05654v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitting to MNRAS; comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.15806">arXiv:2307.15806</a> <span> [<a href="https://arxiv.org/pdf/2307.15806">pdf</a>, <a href="https://arxiv.org/format/2307.15806">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Crowded No More: The Accuracy of the Hubble Constant Tested with High Resolution Observations of Cepheids by JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Wenlong Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Macri%2C+L+M">Lucas M. Macri</a>, <a href="/search/astro-ph?searchtype=author&query=Breuval%2C+L">Louise Breuval</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Perrin%2C+M">Marshall Perrin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.15806v1-abstract-short" style="display: inline;"> High-resolution JWST observations can test confusion-limited HST observations for a photometric bias that could affect extragalactic Cepheids and the determination of the Hubble constant. We present JWST NIRCAM observations in two epochs and three filters of >330 Cepheids in NGC4258 (which has a 1.5% maser-based geometric distance) and in NGC5584 (host of SNIa 2007af), near the median distance of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.15806v1-abstract-full').style.display = 'inline'; document.getElementById('2307.15806v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.15806v1-abstract-full" style="display: none;"> High-resolution JWST observations can test confusion-limited HST observations for a photometric bias that could affect extragalactic Cepheids and the determination of the Hubble constant. We present JWST NIRCAM observations in two epochs and three filters of >330 Cepheids in NGC4258 (which has a 1.5% maser-based geometric distance) and in NGC5584 (host of SNIa 2007af), near the median distance of the SH0ES HST SNIa host sample and with the best leverage among them to detect such a bias. JWST provides far superior source separation from line-of-sight companions than HST in the NIR to largely negate confusion or crowding noise at these wavelengths, where extinction is minimal. The result is a remarkable >2.5x reduction in the dispersion of the Cepheid P-L relations, from 0.45 to 0.17 mag, improving individual Cepheid precision from 20% to 7%. Two-epoch photometry confirmed identifications, tested JWST photometric stability, and constrained Cepheid phases. The P-L relation intercepts are in very good agreement, with differences (JWST-HST) of 0.00+/-0.03 and 0.02+/-0.03 mag for NGC4258 and NGC5584, respectively. The difference in the determination of H_0 between HST and JWST from these intercepts is 0.02+/-0.04 mag, insensitive to JWST zeropoints or count-rate non-linearity thanks to error cancellation between rungs. We explore a broad range of analysis variants (including passband combinations, phase corrections, measured detector offsets, and crowding levels) indicating robust baseline results. These observations provide the strongest evidence yet that systematic errors in HST Cepheid photometry do not play a significant role in the present Hubble Tension. Upcoming JWST observations of >12 SNIa hosts should further refine the local measurement of the Hubble constant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.15806v1-abstract-full').style.display = 'none'; document.getElementById('2307.15806v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">submitted to ApJ, comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.13696">arXiv:2307.13696</a> <span> [<a href="https://arxiv.org/pdf/2307.13696">pdf</a>, <a href="https://arxiv.org/format/2307.13696">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Survey Supernova Program: Cosmological Biases from Host Galaxy Mismatch of Type Ia Supernovae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">H. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+C">C. Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T">T. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Rose%2C+B">B. Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.13696v2-abstract-short" style="display: inline;"> Redshift measurements, primarily obtained from host galaxies, are essential for inferring cosmological parameters from type Ia supernovae (SNe Ia). Matching SNe to host galaxies using images is non-trivial, resulting in a subset of SNe with mismatched hosts and thus incorrect redshifts. We evaluate the host galaxy mismatch rate and resulting biases on cosmological parameters from simulations model… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13696v2-abstract-full').style.display = 'inline'; document.getElementById('2307.13696v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.13696v2-abstract-full" style="display: none;"> Redshift measurements, primarily obtained from host galaxies, are essential for inferring cosmological parameters from type Ia supernovae (SNe Ia). Matching SNe to host galaxies using images is non-trivial, resulting in a subset of SNe with mismatched hosts and thus incorrect redshifts. We evaluate the host galaxy mismatch rate and resulting biases on cosmological parameters from simulations modeled after the Dark Energy Survey 5-Year (DES-SN5YR) photometric sample. For both DES-SN5YR data and simulations, we employ the directional light radius method for host galaxy matching. In our SN Ia simulations, we find that 1.7% of SNe are matched to the wrong host galaxy, with redshift difference between the true and matched host of up to 0.6. Using our analysis pipeline, we determine the shift in the dark energy equation of state parameter (Dw) due to including SNe with incorrect host galaxy matches. For SN Ia-only simulations, we find Dw = 0.0013 +/- 0.0026 with constraints from the cosmic microwave background (CMB). Including core-collapse SNe and peculiar SNe Ia in the simulation, we find that Dw ranges from 0.0009 to 0.0032 depending on the photometric classifier used. This bias is an order of magnitude smaller than the expected total uncertainty on w from the DES-SN5YR sample of around 0.03. We conclude that the bias on w from host galaxy mismatch is much smaller than the uncertainties expected from the DES-SN5YR sample, but we encourage further studies to reduce this bias through better host-matching algorithms or selection cuts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13696v2-abstract-full').style.display = 'none'; document.getElementById('2307.13696v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.09511">arXiv:2307.09511</a> <span> [<a href="https://arxiv.org/pdf/2307.09511">pdf</a>, <a href="https://arxiv.org/format/2307.09511">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Enabling Kilonova Science with Nancy Grace Roman Space Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Andreoni%2C+I">Igor Andreoni</a>, <a href="/search/astro-ph?searchtype=author&query=Coughlin%2C+M+W">Michael W. Coughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Criswell%2C+A+W">Alexander W. Criswell</a>, <a href="/search/astro-ph?searchtype=author&query=Bulla%2C+M">Mattia Bulla</a>, <a href="/search/astro-ph?searchtype=author&query=Toivonen%2C+A">Andrew Toivonen</a>, <a href="/search/astro-ph?searchtype=author&query=Singer%2C+L+P">Leo P. Singer</a>, <a href="/search/astro-ph?searchtype=author&query=Palmese%2C+A">Antonella Palmese</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">E. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Gezari%2C+S">Suvi Gezari</a>, <a href="/search/astro-ph?searchtype=author&query=Kasliwal%2C+M+M">Mansi M. Kasliwal</a>, <a href="/search/astro-ph?searchtype=author&query=Kiendrebeogo%2C+R+W">R. Weizmann Kiendrebeogo</a>, <a href="/search/astro-ph?searchtype=author&query=Mahabal%2C+A">Ashish Mahabal</a>, <a href="/search/astro-ph?searchtype=author&query=Moriya%2C+T+J">Takashi J. Moriya</a>, <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">Armin Rest</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Simcoe%2C+R+A">Robert A. Simcoe</a>, <a href="/search/astro-ph?searchtype=author&query=Soon%2C+J">Jamie Soon</a>, <a href="/search/astro-ph?searchtype=author&query=Stein%2C+R">Robert Stein</a>, <a href="/search/astro-ph?searchtype=author&query=Travouillon%2C+T">Tony Travouillon</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.09511v2-abstract-short" style="display: inline;"> Binary neutron star mergers and neutron star-black hole mergers are multi-messenger sources that can be detected in gravitational waves and in electromagnetic radiation. The low electron fraction of neutron star merger ejecta favors the production of heavy elements such as lanthanides and actinides via rapid neutron capture (r-process). The decay of these unstable nuclei powers an infrared-bright… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.09511v2-abstract-full').style.display = 'inline'; document.getElementById('2307.09511v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.09511v2-abstract-full" style="display: none;"> Binary neutron star mergers and neutron star-black hole mergers are multi-messenger sources that can be detected in gravitational waves and in electromagnetic radiation. The low electron fraction of neutron star merger ejecta favors the production of heavy elements such as lanthanides and actinides via rapid neutron capture (r-process). The decay of these unstable nuclei powers an infrared-bright transient called a "kilonova". The discovery of a population of kilonovae will allow us to determine if neutron star mergers are the dominant sites for r-process element nucleosynthesis, constrain the equation of state of nuclear matter, and make independent measurements of the Hubble constant. The Nancy Grace Roman Space Telescope (Roman) will have a unique combination of depth, near-infrared sensitivity, and wide field of view. These characteristics will enable Roman's discovery of GW counterparts that will be missed by optical telescopes, such as kilonova that are associated with large distances, high lanthanide fractions, high binary mass-ratios, large dust extinction in the line of sight, or that are observed from equatorial viewing angles. Our analysis suggests to (i) make available a rapid (about 1 week) Target of Opportunity mode for GW follow-up; (ii) include observations of the High Latitude Time-Domain survey footprint in at least two filters (preferably the F158 and F213 filters) with a cadence of < 8 days; (iii) operate in synergy with Rubin Observatory. Following these recommendations, we expect that 1-6 kilonovae can be identified by Roman via ToO observations of well localized (A < 10 sq. deg., 90% C.I.) neutron star mergers during 1.5 years of the LIGO-Virgo-KAGRA fifth (or about 4-21 in during the sixth) observing run. A sample of 5-40 serendipitously discovered kilonovae can be collected in a 5-year high latitude survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.09511v2-abstract-full').style.display = 'none'; document.getElementById('2307.09511v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in Astroparticle Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.02670">arXiv:2307.02670</a> <span> [<a href="https://arxiv.org/pdf/2307.02670">pdf</a>, <a href="https://arxiv.org/format/2307.02670">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Roman CCS White Paper: Measuring Type Ia Supernovae Discovered in the Roman High Latitude Time Domain Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hounsell%2C+R">Rebekah Hounsell</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">Dillon Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Rose%2C+B">Benjamin Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Fox%2C+O">Ori Fox</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">Masao Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Macias%2C+P">Phillip Macias</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+B">Bhavin Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Desutua%2C+S">Susana Desutua</a>, <a href="/search/astro-ph?searchtype=author&query=Rubin%2C+D">David Rubin</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Perlmutter%2C+S">Saul Perlmutter</a>, <a href="/search/astro-ph?searchtype=author&query=Aldering%2C+G">Greg Aldering</a>, <a href="/search/astro-ph?searchtype=author&query=Mandel%2C+K">Kaisey Mandel</a>, <a href="/search/astro-ph?searchtype=author&query=Sosey%2C+M">Megan Sosey</a>, <a href="/search/astro-ph?searchtype=author&query=Suzuki%2C+N">Nao Suzuki</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan%2C+R">Russell Ryan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.02670v1-abstract-short" style="display: inline;"> We motivate the cosmological science case of measuring Type Ia supernovae with the Nancy Grace Roman Space Telescope as part of the High Latitude Time Domain Survey. We discuss previously stated requirements for the science, and a baseline survey strategy. We discuss the various areas that must still be optimized and point to the other white papers that consider these topics in detail. Overall, th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.02670v1-abstract-full').style.display = 'inline'; document.getElementById('2307.02670v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.02670v1-abstract-full" style="display: none;"> We motivate the cosmological science case of measuring Type Ia supernovae with the Nancy Grace Roman Space Telescope as part of the High Latitude Time Domain Survey. We discuss previously stated requirements for the science, and a baseline survey strategy. We discuss the various areas that must still be optimized and point to the other white papers that consider these topics in detail. Overall, the baseline case should enable an exquisite measurement of dark energy using SNe Ia from z=0.1 to z>2, and further optimization should only strengthen this once-in-a-generation experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.02670v1-abstract-full').style.display = 'none'; document.getElementById('2307.02670v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.17228">arXiv:2306.17228</a> <span> [<a href="https://arxiv.org/pdf/2306.17228">pdf</a>, <a href="https://arxiv.org/ps/2306.17228">ps</a>, <a href="https://arxiv.org/format/2306.17228">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Roman CCS White Paper: Options to Increase the Coverage Area of Prism Time Series in the High-Latitude Time Domain Core Community Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rose%2C+B">Benjamin Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Gomez%2C+S">Sebastian Gomez</a>, <a href="/search/astro-ph?searchtype=author&query=Hounsell%2C+R">Rebekah Hounsell</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+B">Bhavin Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Rubin%2C+D">David Rubin</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">Masao Sako</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.17228v1-abstract-short" style="display: inline;"> The current reference High-latitude time domain survey increases the completeness of transients with prism temporal time series data by adjusting the ratio of prism-to-imaging time. However, there are two other nobs that allow for a more complete prism coverage: prism cadence and exposure time. In this white paper, we discuss how changes to the prism cadence and exposure time -- in order to increa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17228v1-abstract-full').style.display = 'inline'; document.getElementById('2306.17228v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.17228v1-abstract-full" style="display: none;"> The current reference High-latitude time domain survey increases the completeness of transients with prism temporal time series data by adjusting the ratio of prism-to-imaging time. However, there are two other nobs that allow for a more complete prism coverage: prism cadence and exposure time. In this white paper, we discuss how changes to the prism cadence and exposure time -- in order to increase the fraction of observed transients with spectral time series -- affect supernova cosmology, transient typing and template building, and the study of rare transients. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17228v1-abstract-full').style.display = 'none'; document.getElementById('2306.17228v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to the Roman Core Community Survey call for white papers</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.17226">arXiv:2306.17226</a> <span> [<a href="https://arxiv.org/pdf/2306.17226">pdf</a>, <a href="https://arxiv.org/format/2306.17226">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Roman CCS White Paper: Considerations for Selecting Fields for the Roman High-latitude Time Domain Core Community Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rose%2C+B">Benjamin Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Aldering%2C+G">Greg Aldering</a>, <a href="/search/astro-ph?searchtype=author&query=Hounsell%2C+R">Rebekah Hounsell</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+B">Bhavin Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Rubin%2C+D">David Rubin</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Perlmutter%2C+S">Saul Perlmutter</a>, <a href="/search/astro-ph?searchtype=author&query=Deustua%2C+S">Susana Deustua</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">Masao Sako</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.17226v1-abstract-short" style="display: inline;"> In this white paper, we review five top considerations for selecting locations of the fields of the Roman High-latitude Time Domain Survey. Based on these considerations, we recommend Akari Deep Field South (ADFS)/Euclid Deep Field South (EDFS) in the Southern Hemisphere has it avoids bright stars, has minimal Milky Way dust, is in Roman Continuous viewing zone, overlaps with multiple past and fut… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17226v1-abstract-full').style.display = 'inline'; document.getElementById('2306.17226v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.17226v1-abstract-full" style="display: none;"> In this white paper, we review five top considerations for selecting locations of the fields of the Roman High-latitude Time Domain Survey. Based on these considerations, we recommend Akari Deep Field South (ADFS)/Euclid Deep Field South (EDFS) in the Southern Hemisphere has it avoids bright stars, has minimal Milky Way dust, is in Roman Continuous viewing zone, overlaps with multiple past and future surveys, and minimal zodiacal background variation. In the North, Extended Groth Strip (EGS) is good except for its zodiacal variation and Supernova/Acceleration Probe North (SNAP-N) and European Large Area Infrared Space Observatory Survey-North 1 (ELAIS N-1) are good except for their synergistic archival data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17226v1-abstract-full').style.display = 'none'; document.getElementById('2306.17226v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to the Roman Core Community Survey call for white papers</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.17222">arXiv:2306.17222</a> <span> [<a href="https://arxiv.org/pdf/2306.17222">pdf</a>, <a href="https://arxiv.org/format/2306.17222">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Roman CCS White Paper: Optimizing the HLTDS Cadence at Fixed Depth </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rubin%2C+D">David Rubin</a>, <a href="/search/astro-ph?searchtype=author&query=Rose%2C+B">Ben Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Hounsell%2C+R">Rebekah Hounsell</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">Masao Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Aldering%2C+G">Greg Aldering</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Perlmutter%2C+S">Saul Perlmutter</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.17222v1-abstract-short" style="display: inline;"> The current proposal for the High Latitude Time Domain Survey (HLTDS) is two tiers (wide and deep) of multi-band imaging and prism spectroscopy with a cadence of five days (Rose et al., 2021). The five-day cadence is motivated by the desire to measure mid-redshift SNe where time dilation is modest as well as to better photometrically characterize the transients detected. This white paper does not… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17222v1-abstract-full').style.display = 'inline'; document.getElementById('2306.17222v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.17222v1-abstract-full" style="display: none;"> The current proposal for the High Latitude Time Domain Survey (HLTDS) is two tiers (wide and deep) of multi-band imaging and prism spectroscopy with a cadence of five days (Rose et al., 2021). The five-day cadence is motivated by the desire to measure mid-redshift SNe where time dilation is modest as well as to better photometrically characterize the transients detected. This white paper does not provide a conclusion as to the best cadence for the HLTDS. Rather, it collects a set of considerations that should be used for a careful study of cadence by a future committee optimizing the Roman survey. This study should optimize the HLTDS for both SN Ia cosmology and other transient science. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17222v1-abstract-full').style.display = 'none'; document.getElementById('2306.17222v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.10103">arXiv:2306.10103</a> <span> [<a href="https://arxiv.org/pdf/2306.10103">pdf</a>, <a href="https://arxiv.org/format/2306.10103">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acf4fb">10.3847/1538-4357/acf4fb <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Standardized Luminosity of the Tip of the Red Giant Branch utilizing Multiple Fields in NGC 4258 and the CATs Algorithm </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+S">Siyang Li</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=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+J">Jiaxi Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Wenlong Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachael Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.10103v1-abstract-short" style="display: inline;"> The Tip of the Red Giant Branch provides a luminous standard candle for calibrating distance ladders that reach Type Ia supernova (SN Ia) hosts. However, recent work reveals that tip measurements vary at the $\sim$ 0.1 mag level for different stellar populations and locations within a host, which may lead to inconsistencies along the distance ladder. We pursue a calibration of the tip using 11 Hub… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.10103v1-abstract-full').style.display = 'inline'; document.getElementById('2306.10103v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.10103v1-abstract-full" style="display: none;"> The Tip of the Red Giant Branch provides a luminous standard candle for calibrating distance ladders that reach Type Ia supernova (SN Ia) hosts. However, recent work reveals that tip measurements vary at the $\sim$ 0.1 mag level for different stellar populations and locations within a host, which may lead to inconsistencies along the distance ladder. We pursue a calibration of the tip using 11 Hubble Space Telescope fields around the maser host, NGC 4258, that is consistent with SN Ia hosts by standardizing tip measurements via their contrast ratios. We find $F814W$-band tips that exhibit a full 0.3 mag range and 0.1 mag dispersion. We do not find any correlation between HI column density and the apparent tip to 0.04 $\pm$ 0.03 mag/cm$^{-2}$. We search for a tip-contrast relation (TCR) and measure the TCR within the fields of NGC 4258 of $-0.015\pm0.008$ mag/$R$, where $R$ is the contrast ratio. This value is consistent with the TCR originally discovered in the GHOSTS sample (Wu et al. 2022) of $-0.023\pm0.005$ mag/R. Combining these measurements, we find a global TCR of $-0.021\pm0.004$ mag/R and a calibration of $M_I^{TRGB} = -4.025 \pm 0.035 - (R-4)\times0.021$ mag. We also use stellar models to simulate single age and metallicity stellar populations with [Fe/H] from $-2.0$ to $-0.7$ and ages from 3 Gyr to 12 Gyr and reconstruct the global TCR found here to a factor of $\sim$ 2. This work is combined in a companion analysis with tip measurements of nearby SN Ia hosts to measure $H_0$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.10103v1-abstract-full').style.display = 'none'; document.getElementById('2306.10103v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 June, 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">20 pages, 12 figures, 3 tables. Submitted to ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 956 32 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.00070">arXiv:2306.00070</a> <span> [<a href="https://arxiv.org/pdf/2306.00070">pdf</a>, <a href="https://arxiv.org/format/2306.00070">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Leveraging SN Ia spectroscopic similarity to improve the measurement of $H_0$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Murakami%2C+Y+S">Yukei S. Murakami</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=Stahl%2C+B+E">Benjamin E. Stahl</a>, <a href="/search/astro-ph?searchtype=author&query=Kenworthy%2C+W+D">W. D'Arcy Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Pluck%2C+D+A">Dahne-More A. Pluck</a>, <a href="/search/astro-ph?searchtype=author&query=Macoretta%2C+A">Antonella Macoretta</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">Dillon Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+O">David O. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D+M">Dan M. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Filippenko%2C+A+V">Alexei V. Filippenko</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.00070v1-abstract-short" style="display: inline;"> Recent studies suggest spectroscopic differences explain a fraction of the variation in Type Ia supernova (SN Ia) luminosities after light-curve/color standardization. In this work, (i) we empirically characterize the variations of standardized SN Ia luminosities, and (ii) we use a spectroscopically inferred parameter, SIP, to improve the precision of SNe Ia along the distance ladder and the deter… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.00070v1-abstract-full').style.display = 'inline'; document.getElementById('2306.00070v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.00070v1-abstract-full" style="display: none;"> Recent studies suggest spectroscopic differences explain a fraction of the variation in Type Ia supernova (SN Ia) luminosities after light-curve/color standardization. In this work, (i) we empirically characterize the variations of standardized SN Ia luminosities, and (ii) we use a spectroscopically inferred parameter, SIP, to improve the precision of SNe Ia along the distance ladder and the determination of the Hubble constant ($H_0$). First, we show that the \texttt{Pantheon+} covariance model modestly overestimates the uncertainty of standardized magnitudes by $\sim 7$%, in the parameter space used by the $\texttt{SH0ES}$ Team to measure $H_0$; accounting for this alone yields $H_0 = 73.01 \pm 0.92$ km s$^{-1}$ Mpc$^{-1}$. Furthermore, accounting for spectroscopic similarity between SNe~Ia on the distance ladder reduces their relative scatter to $\sim0.12$ mag per object (compared to $\sim 0.14$ mag previously). Combining these two findings in the model of SN covariance, we find an overall 14% reduction (to $\pm 0.85$km s$^{-1}$ Mpc$^{-1}$) of the uncertainty in the Hubble constant and a modest increase in its value. Including a budget for systematic uncertainties itemized by Riess et al. (2022a), we report an updated local Hubble constant with $\sim1.2$% uncertainty, $H_0 = 73.29 \pm 0.90$km s$^{-1}$ Mpc$^{-1}$. We conclude that spectroscopic differences among photometrically standardized SNe Ia do not explain the ``Hubble tension." Rather, accounting for such differences increases its significance, as the discrepancy against $螞$CDM calibrated by the ${\it Planck}$ 2018 measurement rises to 5.7$蟽$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.00070v1-abstract-full').style.display = 'none'; document.getElementById('2306.00070v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 May, 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">28 pages, 15 figures, accepted to JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.06693">arXiv:2304.06693</a> <span> [<a href="https://arxiv.org/pdf/2304.06693">pdf</a>, <a href="https://arxiv.org/format/2304.06693">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> CATS: The Hubble Constant from Standardized TRGB and Type Ia Supernova Measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">A. G. Riess</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+J">J. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+S">S. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">G. S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">R. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">S. Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R">R. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Dhawan%2C+S">S. Dhawan</a>, <a href="/search/astro-ph?searchtype=author&query=Ke%2C+X">X. Ke</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.06693v1-abstract-short" style="display: inline;"> The Tip of the Red Giant Branch (TRGB) provides a luminous standard candle for constructing distance ladders to measure the Hubble constant. In practice its measurements via edge-detection response (EDR) are complicated by the apparent fuzziness of the tip and the multi-peak landscape of the EDR. As a result, it can be difficult to replicate due to a case-by-case measurement process. Previously we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.06693v1-abstract-full').style.display = 'inline'; document.getElementById('2304.06693v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.06693v1-abstract-full" style="display: none;"> The Tip of the Red Giant Branch (TRGB) provides a luminous standard candle for constructing distance ladders to measure the Hubble constant. In practice its measurements via edge-detection response (EDR) are complicated by the apparent fuzziness of the tip and the multi-peak landscape of the EDR. As a result, it can be difficult to replicate due to a case-by-case measurement process. Previously we optimized an unsupervised algorithm, Comparative Analysis of TRGBs (CATs), to minimize the variance among multiple halo fields per host without reliance on individualized choices, achieving state-of-the-art $\sim$ $<$ 0.05 mag distance measures for optimal data. Further, we found an empirical correlation at 5$蟽$ confidence in the GHOSTS halo survey between our measurements of the tip and their contrast ratios (ratio of stars 0.5 mag just below and above the tip), useful for standardizing the apparent tips at different host locations. Here, we apply this algorithm to an expanded sample of SN Ia hosts to standardize these to multiple fields in the geometric anchor, NGC 4258. In concert with the Pantheon$+$ SN Ia sample, this analysis produces a (baseline) result of $H_0= 73.22 \pm 2.06$ km/s/Mpc. The largest difference in $H_0$ between this and similar studies employing the TRGB derives from corrections for SN survey differences and local flows used in most recent SN Ia compilations but which were absent in earlier studies. SN-related differences total $\sim$ 2.0 km/s/Mpc. A smaller share, $\sim$ 1.4 km/s/Mpc, results from the inhomogeneity of the TRGB calibration across the distance ladder. We employ a grid of 108 variants around the optimal TRGB algorithm and find the median of variants is $72.94\pm1.98$ km/s/Mpc with an additional uncertainty due to algorithm choices of 0.83 km/s/Mpc. None of these TRGB variants result in $H_0$ less than 71.6 km/s/Mpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.06693v1-abstract-full').style.display = 'none'; document.getElementById('2304.06693v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 April, 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">Submitted to ApJL, comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.01858">arXiv:2304.01858</a> <span> [<a href="https://arxiv.org/pdf/2304.01858">pdf</a>, <a href="https://arxiv.org/format/2304.01858">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/acca15">10.3847/1538-3881/acca15 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Survey Supernova Program: Corrections on photometry due to wavelength-dependent atmospheric effects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Acevedo%2C+M">M. Acevedo</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+B">B. Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M">M. Jarvis</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">H. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Lasker%2C+J">J. Lasker</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a> , et al. (42 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="2304.01858v1-abstract-short" style="display: inline;"> Wavelength-dependent atmospheric effects impact photometric supernova flux measurements for ground-based observations. We present corrections on supernova flux measurements from the Dark Energy Survey Supernova Program's 5YR sample (DES-SN5YR) for differential chromatic refraction (DCR) and wavelength-dependent seeing, and we show their impact on the cosmological parameters $w$ and $惟_m$. We use… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.01858v1-abstract-full').style.display = 'inline'; document.getElementById('2304.01858v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.01858v1-abstract-full" style="display: none;"> Wavelength-dependent atmospheric effects impact photometric supernova flux measurements for ground-based observations. We present corrections on supernova flux measurements from the Dark Energy Survey Supernova Program's 5YR sample (DES-SN5YR) for differential chromatic refraction (DCR) and wavelength-dependent seeing, and we show their impact on the cosmological parameters $w$ and $惟_m$. We use $g-i$ colors of Type Ia supernovae (SNe Ia) to quantify astrometric offsets caused by DCR and simulate point spread functions (PSFs) using the GalSIM package to predict the shapes of the PSFs with DCR and wavelength-dependent seeing. We calculate the magnitude corrections and apply them to the magnitudes computed by the DES-SN5YR photometric pipeline. We find that for the DES-SN5YR analysis, not accounting for the astrometric offsets and changes in the PSF shape cause an average bias of $+0.2$ mmag and $-0.3$ mmag respectively, with standard deviations of $0.7$ mmag and $2.7$ mmag across all DES observing bands (\textit{griz}) throughout all redshifts. When the DCR and seeing effects are not accounted for, we find that $w$ and $惟_m$ are lower by less than $0.004\pm0.02$ and $0.001\pm0.01$ respectively, with $0.02$ and $0.01$ being the $1蟽$ statistical uncertainties. Although we find that these biases do not limit the constraints of the DES-SN5YR sample, future surveys with much higher statistics, lower systematics, and especially those that observe in the $u$ band will require these corrections as wavelength-dependent atmospheric effects are larger at shorter wavelengths. We also discuss limitations of our method and how they can be better accounted for in future surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.01858v1-abstract-full').style.display = 'none'; document.getElementById('2304.01858v1-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 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">15 pages, 13 figures, accepted by the Astronomical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DES-2022-0740, FERMILAB-PUB-23-040-PPD </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.05184">arXiv:2302.05184</a> <span> [<a href="https://arxiv.org/pdf/2302.05184">pdf</a>, <a href="https://arxiv.org/format/2302.05184">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Rates and properties of type Ia supernovae in galaxy clusters within the Dark Energy Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Toy%2C+M">M. Toy</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Frohmaier%2C+C">C. Frohmaier</a>, <a href="/search/astro-ph?searchtype=author&query=Graur%2C+O">O. Graur</a>, <a href="/search/astro-ph?searchtype=author&query=Palmese%2C+A">A. Palmese</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Annis%2C+J">J. Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a>, <a href="/search/astro-ph?searchtype=author&query=Kind%2C+M+C">M. Carrasco Kind</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a> , et al. (37 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="2302.05184v2-abstract-short" style="display: inline;"> We identify 66 photometrically classified type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) that have occurred within red-sequence selected galaxy clusters. We compare light-curve and host galaxy properties of the cluster SNe to 1024 DES SNe Ia located in field galaxies, the largest comparison of two such samples at high redshift (z > 0.1). We find that cluster SN light curves decline… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05184v2-abstract-full').style.display = 'inline'; document.getElementById('2302.05184v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.05184v2-abstract-full" style="display: none;"> We identify 66 photometrically classified type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) that have occurred within red-sequence selected galaxy clusters. We compare light-curve and host galaxy properties of the cluster SNe to 1024 DES SNe Ia located in field galaxies, the largest comparison of two such samples at high redshift (z > 0.1). We find that cluster SN light curves decline faster than those in the field (97.7 per cent confidence). However, when limiting these samples to host galaxies of similar colour and mass, there is no significant difference in the SN light curve properties. Motivated by previous detections of a higher-normalised SN Ia delay time distribution in galaxy clusters, we measure the intrinsic rate of SNe Ia in cluster and field environments. We find the average ratio of the SN Ia rate per galaxy between high mass ($10\leq\log\mathrm{(M_{*}/M_{\odot})} \leq 11.25$) cluster and field galaxies to be $0.594 \pm0.068$. This difference is mass-dependent, with the ratio declining with increasing mass, which suggests that the stellar populations in cluster hosts are older than those in field hosts. We show that the mass-normalised rate (or SNe per unit mass) in massive-passive galaxies is consistent between cluster and field environments. Additionally, both of these rates are consistent with rates previously measured in clusters at similar redshifts. We conclude that in massive-passive galaxies, which are the dominant hosts of cluster SNe, the cluster DTD is comparable to the field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05184v2-abstract-full').style.display = 'none'; document.getElementById('2302.05184v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.11868">arXiv:2301.11868</a> <span> [<a href="https://arxiv.org/pdf/2301.11868">pdf</a>, <a href="https://arxiv.org/format/2301.11868">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad1077">10.1093/mnras/stad1077 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The DEHVILS Survey Overview and Initial Data Release: High-Quality Near-Infrared Type Ia Supernova Light Curves at Low Redshift </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+E+R">Erik R. Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+O">David O. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">Bruno O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Do%2C+A">Aaron Do</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=Ward%2C+S+M">Sam M. Ward</a>, <a href="/search/astro-ph?searchtype=author&query=Dwomoh%2C+A">Arianna Dwomoh</a>, <a href="/search/astro-ph?searchtype=author&query=de+Jaeger%2C+T">Thomas de Jaeger</a>, <a href="/search/astro-ph?searchtype=author&query=Jha%2C+S+W">Saurabh W. Jha</a>, <a href="/search/astro-ph?searchtype=author&query=Mandel%2C+K+S">Kaisey S. Mandel</a>, <a href="/search/astro-ph?searchtype=author&query=Pierel%2C+J+D+R">Justin D. R. Pierel</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">Brodie Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Rose%2C+B+M">Benjamin M. Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Rubin%2C+D">David Rubin</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">Benjamin J. Shappee</a>, <a href="/search/astro-ph?searchtype=author&query=Thorp%2C+S">Stephen Thorp</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=Tully%2C+R+B">R. Brent Tully</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">Maria Vincenzi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.11868v2-abstract-short" style="display: inline;"> While the sample of optical Type Ia Supernova (SN Ia) light curves (LCs) usable for cosmological parameter measurements surpasses 2000, the sample of published, cosmologically viable near-infrared (NIR) SN Ia LCs, which have been shown to be good "standard candles," is still $\lesssim$ 200. Here, we present high-quality NIR LCs for 83 SNe Ia ranging from $0.002 < z < 0.09$ as a part of the Dark En… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.11868v2-abstract-full').style.display = 'inline'; document.getElementById('2301.11868v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.11868v2-abstract-full" style="display: none;"> While the sample of optical Type Ia Supernova (SN Ia) light curves (LCs) usable for cosmological parameter measurements surpasses 2000, the sample of published, cosmologically viable near-infrared (NIR) SN Ia LCs, which have been shown to be good "standard candles," is still $\lesssim$ 200. Here, we present high-quality NIR LCs for 83 SNe Ia ranging from $0.002 < z < 0.09$ as a part of the Dark Energy, H$_0$, and peculiar Velocities using Infrared Light from Supernovae (DEHVILS) survey. Observations are taken using UKIRT's WFCAM, where the median depth of the images is 20.7, 20.1, and 19.3 mag (Vega) for $Y$, $J$, and $H$-bands, respectively. The median number of epochs per SN Ia is 18 for all three bands ($YJH$) combined and 6 for each band individually. We fit 47 SN Ia LCs that pass strict quality cuts using three LC models, SALT3, SNooPy, and BayeSN and find scatter on the Hubble diagram to be comparable to or better than scatter from optical-only fits in the literature. Fitting NIR-only LCs, we obtain standard deviations ranging from 0.128-0.135 mag. Additionally, we present a refined calibration method for transforming 2MASS magnitudes to WFCAM magnitudes using HST CALSPEC stars that results in a 0.03 mag shift in the WFCAM $Y$-band magnitudes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.11868v2-abstract-full').style.display = 'none'; document.getElementById('2301.11868v2-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">v1</span> submitted 27 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 9 figures. Accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.10644">arXiv:2301.10644</a> <span> [<a href="https://arxiv.org/pdf/2301.10644">pdf</a>, <a href="https://arxiv.org/format/2301.10644">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad320">10.1093/mnras/stad320 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SALT2 Versus SALT3: Updated Model Surfaces and Their Impacts on Type Ia Supernova Cosmology </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+G">G. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+O">D. O. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+M">M. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Kenworthy%2C+W+D">W. D. Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Pierel%2C+J+D+R">J. D. R. Pierel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.10644v1-abstract-short" style="display: inline;"> For the past decade, SALT2 has been the most common model used to fit Type Ia supernova (SN Ia) light curves for dark energy analyses. Recently, the SALT3 model was released, which upgraded a number of model features but has not yet been used for measurements of dark energy. Here, we evaluate the impact of switching from SALT2 to SALT3 for a SN cosmology analysis. We train SALT2 and SALT3 on an id… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.10644v1-abstract-full').style.display = 'inline'; document.getElementById('2301.10644v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.10644v1-abstract-full" style="display: none;"> For the past decade, SALT2 has been the most common model used to fit Type Ia supernova (SN Ia) light curves for dark energy analyses. Recently, the SALT3 model was released, which upgraded a number of model features but has not yet been used for measurements of dark energy. Here, we evaluate the impact of switching from SALT2 to SALT3 for a SN cosmology analysis. We train SALT2 and SALT3 on an identical training sample of 1083 well-calibrated Type Ia supernovae, ensuring that any differences found come from the underlying model framework. We publicly release the results of this training (the SALT "surfaces"). We then run a cosmology analysis on the public Dark Energy Survey 3-Year Supernova data sample (DES-SN3YR), and on realistic simulations of those data. We provide the first estimate of the SN+CMB systematic uncertainty arising from the choice of SALT model framework (i.e. SALT2 versus SALT3), $螖w = +0.001 \pm 0.005$ -- a negligible effect at the current level of dark energy analyses. We also find that the updated surfaces are less sensitive to photometric calibration uncertainties than previous SALT2 surfaces, with the average spectral energy density dispersion reduced by a factor of two over optical wavelengths. This offers an opportunity to reduce the contribution of calibration errors to SN cosmology uncertainty budgets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.10644v1-abstract-full').style.display = 'none'; document.getElementById('2301.10644v1-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 13 figures, accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.06879">arXiv:2212.06879</a> <span> [<a href="https://arxiv.org/pdf/2212.06879">pdf</a>, <a href="https://arxiv.org/format/2212.06879">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/acd051">10.3847/1538-4365/acd051 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Propagating Uncertainties in the SALT3 Model Training Process to Cosmological Constraints </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dai%2C+M">M. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+O">D. O. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Kenworthy%2C+W+D">W. D. Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Pierel%2C+J+D+R">J. D. R. Pierel</a>, <a href="/search/astro-ph?searchtype=author&query=Foley%2C+R+J">R. J. Foley</a>, <a href="/search/astro-ph?searchtype=author&query=Jha%2C+S+W">S. W. Jha</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D+M">D. M. Scolnic</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="2212.06879v2-abstract-short" style="display: inline;"> Type Ia supernovae (SNe Ia) are standardizable candles that must be modeled empirically to yield cosmological constraints. To understand the robustness of this modeling to variations in the model training procedure, we build an end-to-end pipeline to test the recently developed SALT3 model. We explore the consequences of removing pre-2000s low-$z$ or poorly calibrated $U$-band data, adjusting the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.06879v2-abstract-full').style.display = 'inline'; document.getElementById('2212.06879v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.06879v2-abstract-full" style="display: none;"> Type Ia supernovae (SNe Ia) are standardizable candles that must be modeled empirically to yield cosmological constraints. To understand the robustness of this modeling to variations in the model training procedure, we build an end-to-end pipeline to test the recently developed SALT3 model. We explore the consequences of removing pre-2000s low-$z$ or poorly calibrated $U$-band data, adjusting the amount and fidelity of SN Ia spectra, and using a model-independent framework to simulate the training data. We find the SALT3 model surfaces are improved by having additional spectra and $U$-band data, and can be shifted by $\sim 5\%$ if host galaxy contamination is not sufficiently removed from SN spectra. We find that resulting measurements of $w$ are consistent to within $2.5\%$ for all training variants explored in this work, with the largest shifts coming from variants that add color-dependent calibration offsets or host galaxy contamination to the training spectra, and those that remove pre-2000s low-$z$ data. These results demonstrate that the SALT3 model training procedure is largely robust to reasonable variations in the training data, but that additional attention must be paid to the treatment of spectroscopic data in the training process. We also find that the training procedure is sensitive to the color distributions of the input data; the resulting $w$ measurement can be biased by $\sim2\%$ if the color distribution is not sufficiently wide. Future low-$z$ data, particularly $u$-band observations and high signal-to-noise ratio SN Ia spectra, will help to significantly improve SN Ia modeling in the coming years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.06879v2-abstract-full').style.display = 'none'; document.getElementById('2212.06879v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">17 pages, 10 figures. Published in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.14291">arXiv:2211.14291</a> <span> [<a href="https://arxiv.org/pdf/2211.14291">pdf</a>, <a href="https://arxiv.org/format/2211.14291">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202346534">10.1051/0004-6361/202346534 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Sample of Dust Attenuation Laws for DES Supernova Host Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Duarte%2C+J">J. Duarte</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Gait%C3%A1n%2C+S">S. Gonz谩lez-Gait谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Mourao%2C+A">A. Mourao</a>, <a href="/search/astro-ph?searchtype=author&query=Paulino-Afonso%2C+A">A. Paulino-Afonso</a>, <a href="/search/astro-ph?searchtype=author&query=Guilherme-Garcia%2C+P">P. Guilherme-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Aguas%2C+J">J. Aguas</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Palmese%2C+A">A. Palmese</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Pieres%2C+A">A. Pieres</a>, <a href="/search/astro-ph?searchtype=author&query=Malag%C3%B3n%2C+A+A+P">A. A. Plazas Malag贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a>, <a href="/search/astro-ph?searchtype=author&query=To%2C+C">C. To</a>, <a href="/search/astro-ph?searchtype=author&query=Gruen%2C+D">D. Gruen</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Gerdes%2C+D+W">D. W. Gerdes</a>, <a href="/search/astro-ph?searchtype=author&query=James%2C+D+J">D. J. James</a>, <a href="/search/astro-ph?searchtype=author&query=Hollowood%2C+D+L">D. L. Hollowood</a>, <a href="/search/astro-ph?searchtype=author&query=Friedel%2C+D">D. Friedel</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.14291v2-abstract-short" style="display: inline;"> Type Ia supernovae (SNe Ia) are useful distance indicators in cosmology, provided their luminosity is standardized by applying empirical corrections based on light-curve properties. One factor behind these corrections is dust extinction, accounted for in the color-luminosity relation of the standardization. This relation is usually assumed to be universal, which could potentially introduce systema… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.14291v2-abstract-full').style.display = 'inline'; document.getElementById('2211.14291v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.14291v2-abstract-full" style="display: none;"> Type Ia supernovae (SNe Ia) are useful distance indicators in cosmology, provided their luminosity is standardized by applying empirical corrections based on light-curve properties. One factor behind these corrections is dust extinction, accounted for in the color-luminosity relation of the standardization. This relation is usually assumed to be universal, which could potentially introduce systematics into the standardization. The ``mass-step'' observed for SNe Ia Hubble residuals has been suggested as one such systematic. We seek to obtain a completer view of dust attenuation properties for a sample of 162 SN Ia host galaxies and to probe their link to the ``mass-step''. We infer attenuation laws towards hosts from both global and local (4 kpc) Dark Energy Survey photometry and Composite Stellar Population model fits. We recover a optical depth/attenuation slope relation, best explained by differing star/dust geometry for different galaxy orientations, which is significantly different from the optical depth/extinction slope relation observed directly for SNe. We obtain a large variation of attenuation slopes and confirm these change with host properties, like stellar mass and age, meaning a universal SN Ia correction should ideally not be assumed. Analyzing the cosmological standardization, we find evidence for a ``mass-step'' and a two dimensional ``dust-step'', both more pronounced for red SNe. Although comparable, the two steps are found no to be completely analogous. We conclude that host galaxy dust data cannot fully account for the ``mass-step'', using either an alternative SN standardization with extinction proxied by host attenuation or a ``dust-step'' approach. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.14291v2-abstract-full').style.display = 'none'; document.getElementById('2211.14291v2-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 10 figues, 9 tables. Supplementary material included (10 pages). Accepted for publication on A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DES-2022-0694; FERMILAB-PUB-22-760-PPD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 680, A56 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.06895">arXiv:2211.06895</a> <span> [<a href="https://arxiv.org/pdf/2211.06895">pdf</a>, <a href="https://arxiv.org/format/2211.06895">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Measuring the Ejecta Velocities of Type Ia Supernovae from the Pan-STARRS1 Medium Deep Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Y+-">Y. -C. Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Jheng%2C+Y+-">Y. -S. Jheng</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+O">D. O. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+I+-">I. -Y. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Foley%2C+R+J">R. J. Foley</a>, <a href="/search/astro-ph?searchtype=author&query=Chornock%2C+R">R. Chornock</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D+M">D. M. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+E">E. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Challis%2C+P+M">P. M. Challis</a>, <a href="/search/astro-ph?searchtype=author&query=Drout%2C+M">M. Drout</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+M+E">M. E. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Kirshner%2C+R+P">R. P. Kirshner</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Lunnan%2C+R">R. Lunnan</a>, <a href="/search/astro-ph?searchtype=author&query=Narayan%2C+G">G. Narayan</a>, <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">A. Rest</a>, <a href="/search/astro-ph?searchtype=author&query=Rodney%2C+S">S. Rodney</a>, <a href="/search/astro-ph?searchtype=author&query=Smartt%2C+S">S. Smartt</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.06895v2-abstract-short" style="display: inline;"> There is growing evidence that Type Ia supernovae (SNe Ia) may originate from multiple explosion channels. Previous studies have indicated that the ejecta velocity of SNe Ia is one powerful tool to discriminate between different channels. In this work, we study ~400 confirmed SNe Ia discovered by the Pan-STARRS1 Medium Deep Survey (PS1-MDS), and obtain a sample of ~50 SNe Ia that have near-peak Si… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.06895v2-abstract-full').style.display = 'inline'; document.getElementById('2211.06895v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.06895v2-abstract-full" style="display: none;"> There is growing evidence that Type Ia supernovae (SNe Ia) may originate from multiple explosion channels. Previous studies have indicated that the ejecta velocity of SNe Ia is one powerful tool to discriminate between different channels. In this work, we study ~400 confirmed SNe Ia discovered by the Pan-STARRS1 Medium Deep Survey (PS1-MDS), and obtain a sample of ~50 SNe Ia that have near-peak Si II 6355 velocity (Vsi) measurements. We investigate the relationships between Vsi and various parameters, including SN light-curve width, color, host-galaxy properties, and redshift. No significant trends are identified between Vsi and light-curve parameters. Regarding the host-galaxy properties, we see a significant trend that high-velocity (HV) SNe Ia (Vsi > 12000 km/s) tend to reside in more massive galaxies compared to normal-velocity (NV) SNe Ia (Vsi < 12000 km/s) when combining both the PS1-MDS dataset and those from previous low-z studies. While we do not see a significant trend between Vsi and redshift, HV SNe Ia appear to be more prevalent in low-z samples than in high-z samples. We discuss several possibilities that could potentially contribute to this trend. Furthermore, we investigate the potential bias on SN Ia distances and find no significant difference in Hubble residuals between HV and NV subgroups. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.06895v2-abstract-full').style.display = 'none'; document.getElementById('2211.06895v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 13 figures, 3 tables, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.06354">arXiv:2211.06354</a> <span> [<a href="https://arxiv.org/pdf/2211.06354">pdf</a>, <a href="https://arxiv.org/format/2211.06354">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acdd7b">10.3847/1538-4357/acdd7b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Comparative Analysis of TRGBs (CATs) from Unsupervised, Multi-Halo-Field Measurements: Contrast is Key </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wu%2C+J">J. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">A. G. Riess</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">G. S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">R. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">S. Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Ke%2C+X">X. Ke</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+S">S. Li</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.06354v1-abstract-short" style="display: inline;"> The Tip of the Red Giant Branch (TRGB) is an apparent discontinuity in the color-magnitude diagram (CMD) along the giant branch due to the end of the red giant evolutionary phase and is used to measure distances in the local universe. In practice, the tip is often fuzzy and its localization via edge detection response (EDR) relies on several methods applied on a case-by-case basis. It is hard to e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.06354v1-abstract-full').style.display = 'inline'; document.getElementById('2211.06354v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.06354v1-abstract-full" style="display: none;"> The Tip of the Red Giant Branch (TRGB) is an apparent discontinuity in the color-magnitude diagram (CMD) along the giant branch due to the end of the red giant evolutionary phase and is used to measure distances in the local universe. In practice, the tip is often fuzzy and its localization via edge detection response (EDR) relies on several methods applied on a case-by-case basis. It is hard to evaluate how individual choices affect a distance estimation using only a single host field while also avoiding confirmation bias. To devise a standardized approach, we compare unsupervised, algorithmic analyses of the TRGB in multiple halo fields per galaxy, up to 11 fields for a single host and 50 fields across 10 galaxies, using high signal-to-noise stellar photometry obtained by the GHOSTS survey with the Hubble Space Telescope. We first optimize methods for the lowest field-to-field dispersion including spatial filtering to remove star forming regions, smoothing and weighting of the luminosity function, selection of the RGB by color, and tip selection based on the number of likely RGB stars and the ratio of stars above versus below the tip ($R$). We find $R$, which we call the tip `contrast', to be the most important indicator of the quality of EDR measurements; we find that field-to-field EDR repeatability varies from 0.3 mag to $\leq$ 0.05 mag for $R=4$ to 7, respectively, though less than half the fields reach the higher quality. Further, we find that $R$, which varies with the age/metallicity of the stellar population based on models, correlates with the magnitude of the tip (and after accounting for low internal extinction), i.e., a tip-contrast relation with slope of $-0.023\pm0.0046$ mag/ratio, a $\sim 5蟽$ result that improves standardization of the TRGB. We discuss the value of consistent TRGB standardization across rungs for robust distance ladder measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.06354v1-abstract-full').style.display = 'none'; document.getElementById('2211.06354v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJ. Comments welcomed</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.01206">arXiv:2211.01206</a> <span> [<a href="https://arxiv.org/pdf/2211.01206">pdf</a>, <a href="https://arxiv.org/format/2211.01206">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad2179">10.1093/mnras/stad2179 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Type Ia Supernova cosmology combining data from the $Euclid$ mission and the Vera C. Rubin Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+A">A. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+-">J. -C. Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Rhodes%2C+J">J. Rhodes</a>, <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+E+R">E. R. Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.01206v1-abstract-short" style="display: inline;"> The $Euclid$ mission will provide first-of-its-kind coverage in the near-infrared over deep (three fields, $\sim$10-20 square degrees each) and wide ($\sim$10000 square degrees) fields. While the survey is not designed to discover transients, the deep fields will have repeated observations over a two-week span, followed by a gap of roughly six months. In this analysis, we explore how useful the de… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.01206v1-abstract-full').style.display = 'inline'; document.getElementById('2211.01206v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.01206v1-abstract-full" style="display: none;"> The $Euclid$ mission will provide first-of-its-kind coverage in the near-infrared over deep (three fields, $\sim$10-20 square degrees each) and wide ($\sim$10000 square degrees) fields. While the survey is not designed to discover transients, the deep fields will have repeated observations over a two-week span, followed by a gap of roughly six months. In this analysis, we explore how useful the deep field observations will be for measuring properties of Type Ia supernovae (SNe Ia). Using simulations that include $Euclid$'s planned depth, area and cadence in the deep fields, we calculate that more than 3700 SNe between $0.0<z<1.5$ will have at least five $Euclid$ detections around peak with signal-to-noise ratio larger than 3. While on their own, $Euclid$ light curves are not good enough to directly constrain distances, when combined with LSST deep field observations, we find that uncertainties on SN distances are reduced by 20-30% for $z<0.8$ and by 40-50% for $z>0.8$. Furthermore, we predict how well additional $Euclid$ mock data can be used to constrain a key systematic in SN Ia studies - the size of the luminosity 'step' found between SNe hosted in high mass ($>10^{10} M_{\odot}$) and low mass ($>10^{10} M_{\odot}$) galaxies. This measurement has unique information in the rest-frame NIR. We predict that if the step is caused by dust, we will be able to measure its reduction in the NIR compared to optical at the 4$蟽$ level. We highlight that the LSST and $Euclid$ observing strategies used in this work are still provisional and some level of joint processing is required. Still, these first results are promising, and assuming $Euclid$ begins observations well before the Nancy Roman Space Telescope (Roman), we expect this dataset to be extremely helpful for preparation for Roman itself. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.01206v1-abstract-full').style.display = 'none'; document.getElementById('2211.01206v1-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 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Scolnic%2C+D&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> 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