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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=Riess%2C+A+G&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Riess%2C+A+G&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Riess%2C+A+G&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Riess%2C+A+G&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Riess%2C+A+G&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a href="/search/?searchtype=author&query=Riess%2C+A+G&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/2502.17438">arXiv:2502.17438</a> <span> [<a href="https://arxiv.org/pdf/2502.17438">pdf</a>, <a href="https://arxiv.org/format/2502.17438">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="History and Philosophy of Physics">physics.hist-ph</span> </div> </div> <p class="title is-5 mathjax"> The Legacy of Henrietta Leavitt: A Re-analysis of the First Cepheid Period-Luminosity Relation </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=Huang%2C+C+D">Caroline D. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</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="2502.17438v1-abstract-short" style="display: inline;"> Henrietta Swan Leavitt's discovery of the relationship between the period and luminosity (hereafter the Leavitt Law) of 25 variable stars in the Small Magellanic Cloud, published in 1912, revolutionized cosmology. These variables, eventually identified as Cepheids, became the first known "standard candles" for measuring extragalactic distances and remain the gold standard for this task today. Leav… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.17438v1-abstract-full').style.display = 'inline'; document.getElementById('2502.17438v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.17438v1-abstract-full" style="display: none;"> Henrietta Swan Leavitt's discovery of the relationship between the period and luminosity (hereafter the Leavitt Law) of 25 variable stars in the Small Magellanic Cloud, published in 1912, revolutionized cosmology. These variables, eventually identified as Cepheids, became the first known "standard candles" for measuring extragalactic distances and remain the gold standard for this task today. Leavitt measured light curves, periods, and minimum and maximum magnitudes from painstaking visual inspection of photographic plates. Her work paved the way for the first precise series of distance measurements that helped set the scale of the Universe, and later the discovery of its expansion by Edwin Hubble in 1929. Here, we re-analyze Leavitt's first Period-Luminosity relation using observations of the same set of stars but with modern data and methods of Cepheid analysis. Using only data from Leavitt's notebooks, we assess the quality of her light curves, measured periods, and the slope and scatter of her Period-Luminosity relations. We show that modern data and methods, for the same objects, reduce the scatter of the Period-Luminosity relation by a factor of two. We also find a bias brightward at the short period end, due to the non-linearity of the plates and environmental crowding. Overall, Leavitt's results are in excellent agreement with contemporary measurements, reinforcing the value of Cepheids in cosmology today, a testament to the enduring quality of her work. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.17438v1-abstract-full').style.display = 'none'; document.getElementById('2502.17438v1-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 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">12 pages, 8 figures. Submitted to PASP. 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/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/2411.07974">arXiv:2411.07974</a> <span> [<a href="https://arxiv.org/pdf/2411.07974">pdf</a>, <a href="https://arxiv.org/format/2411.07974">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Hubble constant anchor galaxy NGC 4258: metallicity and distance from blue supergiants </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kudritzki%2C+R">Rolf-Peter Kudritzki</a>, <a href="/search/astro-ph?searchtype=author&query=Urbaneja%2C+M+A">Miguel A. Urbaneja</a>, <a href="/search/astro-ph?searchtype=author&query=Bresolin%2C+F">Fabio Bresolin</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=Yuan%2C+W">Wenlong Yuan</a>, <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> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.07974v1-abstract-short" style="display: inline;"> A quantitative spectroscopic study of blue supergiant stars in the Hubble constant anchor galaxy NGC 4258 is presented. The non-LTE analysis of Keck I telescope LRIS spectra yields a central logarithmic metallicity (in units of the solar value) of [Z] = -0.05\pm0.05 and a very shallow gradient of -(0.09\pm0.11)r/r25 with respect to galactocentric distance in units of the isophotal radius. Good agr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07974v1-abstract-full').style.display = 'inline'; document.getElementById('2411.07974v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.07974v1-abstract-full" style="display: none;"> A quantitative spectroscopic study of blue supergiant stars in the Hubble constant anchor galaxy NGC 4258 is presented. The non-LTE analysis of Keck I telescope LRIS spectra yields a central logarithmic metallicity (in units of the solar value) of [Z] = -0.05\pm0.05 and a very shallow gradient of -(0.09\pm0.11)r/r25 with respect to galactocentric distance in units of the isophotal radius. Good agreement with the mass-metallicity relationship of star forming galaxies based on stellar absorption line studies is found. A comparison with HII region oxygen abundances obtained from the analysis of strong emission lines shows reasonable agreement when the Pettini & Pagel (2004) calibration is used, while the Zaritsky et al. (1994) calibration yields values that are 0.2 to 0.3 dex larger. These results allow to put the metallicity calibration of the Cepheid Period--Luminosity relation in this anchor galaxy on a purely stellar basis. Interstellar reddening and extinction are determined using HST and JWST photometry. Based on extinction-corrected magnitudes, combined with the stellar effective temperatures and gravities we determine, we use the Flux-weighted Gravity--Luminosity Relationship (FGLR) to estimate an independent spectroscopic distance. We obtain a distance modulus m-M = 29.38\pm0.12 mag, in agreement with the geometrical distance derived from the analysis of the water maser orbits in the galaxy's central circumnuclear disk. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07974v1-abstract-full').style.display = 'none'; document.getElementById('2411.07974v1-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/2408.00065">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/2405.12297">arXiv:2405.12297</a> <span> [<a href="https://arxiv.org/pdf/2405.12297">pdf</a>, <a href="https://arxiv.org/format/2405.12297">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> HST/JWST Long-Term Monitoring Working Group Final Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jha%2C+S+W">Saurabh W. Jha</a>, <a href="/search/astro-ph?searchtype=author&query=Casetti-Dinescu%2C+D+I">Dana I. Casetti-Dinescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bernstein%2C+G+M">Gary M. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Hayes%2C+M+J">Matthew J. Hayes</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">Lidia M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Pace%2C+A+B">Andrew B. Pace</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">Robert M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Reiter%2C+M">Megan Reiter</a>, <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">Armin Rest</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=Sand%2C+D+J">David J. Sand</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</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="2405.12297v2-abstract-short" style="display: inline;"> The Astro2020 Decadal Survey recognizes time-domain astronomy as a key science area over the next decade and beyond. With over 30 years of HST data and the potential for 20 years of JWST operations, these flagship observatories offer an unparalleled prospect for a half-century of space-based observations in the time domain. To take best advantage of this opportunity, STScI charged a working group… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12297v2-abstract-full').style.display = 'inline'; document.getElementById('2405.12297v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.12297v2-abstract-full" style="display: none;"> The Astro2020 Decadal Survey recognizes time-domain astronomy as a key science area over the next decade and beyond. With over 30 years of HST data and the potential for 20 years of JWST operations, these flagship observatories offer an unparalleled prospect for a half-century of space-based observations in the time domain. To take best advantage of this opportunity, STScI charged a working group to solicit community input and formulate strategies to maximize the science return in time-domain astronomy from these two platforms. Here, the HST/JWST Long-Term Monitoring Working Group reports on the input we received and presents our recommendations to enhance the scientific return for time-domain astronomy from HST and JWST. We suggest changes in policies to enable and prioritize long-term science programs of high scientific value. As charged, we also develop recommendations based on community input for a JWST Director's Discretionary Time program to observe high-redshift transients. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12297v2-abstract-full').style.display = 'none'; document.getElementById('2405.12297v2-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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, 3 figures, minor typos corrected, working group information at https://outerspace.stsci.edu/display/HPR/Long-term+variability+monitoring+strategies+for+HST+and+JWST</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.08038">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/2403.18954">arXiv:2403.18954</a> <span> [<a href="https://arxiv.org/pdf/2403.18954">pdf</a>, <a href="https://arxiv.org/format/2403.18954">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/ad3c43">10.3847/1538-4357/ad3c43 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JWST Photometric Time-Delay and Magnification Measurements for the Triply-Imaged Type Ia "Supernova H0pe" at z = 1.78 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Frye%2C+B+L">B. L. Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Pascale%2C+M">M. Pascale</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Dhawan%2C+S">S. Dhawan</a>, <a href="/search/astro-ph?searchtype=author&query=Gilman%2C+D">D. Gilman</a>, <a href="/search/astro-ph?searchtype=author&query=Grayling%2C+M">M. Grayling</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+S">S. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Kelly%2C+P">P. Kelly</a>, <a href="/search/astro-ph?searchtype=author&query=Thorp%2C+S">S. Thorp</a>, <a href="/search/astro-ph?searchtype=author&query=Arendse%2C+N">N. Arendse</a>, <a href="/search/astro-ph?searchtype=author&query=Birrer%2C+S">S. Birrer</a>, <a href="/search/astro-ph?searchtype=author&query=Bronikowski%2C+M">M. Bronikowski</a>, <a href="/search/astro-ph?searchtype=author&query=Canameras%2C+R">R. Canameras</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">D. Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">S. H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">S. P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Dsilva%2C+J+C+J">J. C. J. Dsilva</a>, <a href="/search/astro-ph?searchtype=author&query=Engesser%2C+M">M. Engesser</a>, <a href="/search/astro-ph?searchtype=author&query=Foo%2C+N">N. Foo</a>, <a href="/search/astro-ph?searchtype=author&query=Gall%2C+C">C. Gall</a>, <a href="/search/astro-ph?searchtype=author&query=Garuda%2C+N">N. Garuda</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a> , et al. (38 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.18954v2-abstract-short" style="display: inline;"> Supernova (SN) H0pe is a gravitationally lensed, triply-imaged, Type Ia SN (SN Ia) discovered in James Webb Space Telescope imaging of the PLCK G165.7+67.0 cluster of galaxies. Well-observed multiply-imaged SNe provide a rare opportunity to constrain the Hubble constant ($H_0$), by measuring the relative time delay between the images and modeling the foreground mass distribution. SN H0pe is locate… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18954v2-abstract-full').style.display = 'inline'; document.getElementById('2403.18954v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.18954v2-abstract-full" style="display: none;"> Supernova (SN) H0pe is a gravitationally lensed, triply-imaged, Type Ia SN (SN Ia) discovered in James Webb Space Telescope imaging of the PLCK G165.7+67.0 cluster of galaxies. Well-observed multiply-imaged SNe provide a rare opportunity to constrain the Hubble constant ($H_0$), by measuring the relative time delay between the images and modeling the foreground mass distribution. SN H0pe is located at $z=1.783$, and is the first SN Ia with sufficient light curve sampling and long enough time delays for an $H_0$ inference. Here we present photometric time-delay measurements and SN properties of SN H0pe. Using JWST/NIRCam photometry we measure time delays of $螖t_{ab}=-116.6^{+10.8}_{-9.3}$ and $螖t_{cb}=-48.6^{+3.6}_{-4.0}$ observer-frame days relative to the last image to arrive (image 2b; all uncertainties are $1蟽$), which corresponds to a $\sim5.6\%$ uncertainty contribution for $H_0$ assuming $70 \rm{km s^{-1} Mpc^{-1}}$. We also constrain the absolute magnification of each image to $渭_{a}=4.3^{+1.6}_{-1.8}$, $渭_{b}=7.6^{+3.6}_{-2.6}$, $渭_{c}=6.4^{+1.6}_{-1.5}$ by comparing the observed peak near-IR magnitude of SN H0pe to the non-lensed population of SNe Ia. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18954v2-abstract-full').style.display = 'none'; document.getElementById('2403.18954v2-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 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 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/2403.18902">arXiv:2403.18902</a> <span> [<a href="https://arxiv.org/pdf/2403.18902">pdf</a>, <a href="https://arxiv.org/format/2403.18902">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"> SN H0pe: The First Measurement of $H_0$ from a Multiply-Imaged Type Ia Supernova, Discovered by JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pascale%2C+M">Massimo Pascale</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B+L">Brenda L. Frye</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=Chen%2C+W">Wenlei Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Kelly%2C+P+L">Patrick L. Kelly</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">Seth H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R+A">Rogier A. Windhorst</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=Kamieneski%2C+P+S">Patrick S. Kamieneski</a>, <a href="/search/astro-ph?searchtype=author&query=Diego%2C+J+M">Jose M. Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Meena%2C+A+K">Ashish K. Meena</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sangjun Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Oguri%2C+M">Masamune Oguri</a>, <a href="/search/astro-ph?searchtype=author&query=Zitrin%2C+A">Adi Zitrin</a>, <a href="/search/astro-ph?searchtype=author&query=Jee%2C+M+J">M. James Jee</a>, <a href="/search/astro-ph?searchtype=author&query=Foo%2C+N">Nicholas Foo</a>, <a href="/search/astro-ph?searchtype=author&query=Leimbach%2C+R">Reagen Leimbach</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+L">Liang Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Goobar%2C+A">Ariel Goobar</a>, <a href="/search/astro-ph?searchtype=author&query=Siebert%2C+M+R">Matthew R. Siebert</a>, <a href="/search/astro-ph?searchtype=author&query=Strolger%2C+L">Lou Strolger</a>, <a href="/search/astro-ph?searchtype=author&query=Willner%2C+S+P">S. P. Willner</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="2403.18902v2-abstract-short" style="display: inline;"> The first James Webb Space Telescope ({\it JWST}) Near InfraRed Camera (NIRCam) imaging in the field of the galaxy cluster PLCK G165.7+67.0 ($z=0.35$) uncovered a Type Ia supernova (SN Ia) at $z=1.78$, called ``SN H0pe." Three different images of this one SN were detected as a result of strong gravitational lensing, each one traversing a different path in spacetime, thereby inducing a relative del… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18902v2-abstract-full').style.display = 'inline'; document.getElementById('2403.18902v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.18902v2-abstract-full" style="display: none;"> The first James Webb Space Telescope ({\it JWST}) Near InfraRed Camera (NIRCam) imaging in the field of the galaxy cluster PLCK G165.7+67.0 ($z=0.35$) uncovered a Type Ia supernova (SN Ia) at $z=1.78$, called ``SN H0pe." Three different images of this one SN were detected as a result of strong gravitational lensing, each one traversing a different path in spacetime, thereby inducing a relative delay in the arrival of each image. Follow-up {\it JWST} observations of all three SN images enabled photometric and rare spectroscopic measurements of the two relative time delays. Following strict blinding protocols which oversaw a live unblinding and regulated post-unblinding changes, these two measured time delays were compared to the predictions of seven independently constructed cluster lens models to measure a value for the Hubble constant, $H_0=71.8^{+9.2}_{-8.1}$ km s$^{-1}$ Mpc$^{-1}$. The range of admissible $H_0$ values predicted across the lens models limits further precision, reflecting the well-known degeneracies between lens model constraints and time delays. It has long been theorized that a way forward is to leverage a standard candle, but this has not been realized until now. For the first time, the lens models are evaluated by their agreement with the SN absolute magnifications, breaking degeneracies and producing our best estimate, $H_0=75.7^{+8.1}_{-5.5}$ km s$^{-1}$ Mpc$^{-1}$. This is the first precision measurement of $H_0$ from a multiply-imaged SN Ia and only the second from any multiply-imaged SN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18902v2-abstract-full').style.display = 'none'; document.getElementById('2403.18902v2-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 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 to ApJ. 27 pages, 7 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/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/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/2312.08423">arXiv:2312.08423</a> <span> [<a href="https://arxiv.org/pdf/2312.08423">pdf</a>, <a href="https://arxiv.org/format/2312.08423">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/ad1ff8">10.3847/1538-4357/ad1ff8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Mira Distance to M101 and a 4% Measurement of H0 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Huang%2C+C+D">Caroline D. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Wenlong Yuan</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=Hack%2C+W">Warren Hack</a>, <a href="/search/astro-ph?searchtype=author&query=Whitelock%2C+P+A">Patricia A. Whitelock</a>, <a href="/search/astro-ph?searchtype=author&query=Zakamska%2C+N+L">Nadia L. Zakamska</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=Marengo%2C+M">Massimo Marengo</a>, <a href="/search/astro-ph?searchtype=author&query=Menzies%2C+J+W">John W. Menzies</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R+K">Randall K. Smith</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.08423v2-abstract-short" style="display: inline;"> The giant spiral galaxy M101 is host to the nearest recent Type Ia Supernova (SN 2011fe) and thus has been extensively monitored in the near-infrared to study the late-time lightcurve of the supernova. Leveraging this existing baseline of observations, we derive the first Mira-based distance to M101 by discovering and classifying a sample of 211 Miras with periods ranging from 240 to 400 days in t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08423v2-abstract-full').style.display = 'inline'; document.getElementById('2312.08423v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.08423v2-abstract-full" style="display: none;"> The giant spiral galaxy M101 is host to the nearest recent Type Ia Supernova (SN 2011fe) and thus has been extensively monitored in the near-infrared to study the late-time lightcurve of the supernova. Leveraging this existing baseline of observations, we derive the first Mira-based distance to M101 by discovering and classifying a sample of 211 Miras with periods ranging from 240 to 400 days in the supernova field. Combined with new HST WFC3/IR channel observations, our dataset totals 11 epochs of F110W (HST $YJ$) and 13 epochs of F160W (HST $H$) data spanning $\sim$2900 days. We adopt absolute calibrations of the Mira Period-Luminosity Relation based on geometric distances to the Large Magellanic Cloud and the water megamaser host galaxy NGC 4258, and find $渭_{\rm M101} = $ 29.10 $\pm$ 0.06 mag. This distance is in 1$蟽$ agreement with most other recent Cepheid and Tip of the Red Giant Branch distance measurements to M101. Including the previous Mira-SNIa host, NGC 1559 and SN 2005df, we determine the fiducial SN Ia peak luminosity, $M^0_B = -19.27 \pm 0.09$ mag. With the Hubble diagram of SNe Ia, we derive $H_0 = 72.37 \pm 2.97 $ km s$^{-1}$Mpc$^{-1}$, a $4.1\%$ measurement of $H_0$ using Miras. We find excellent agreement with recent Cepheid distance ladder measurements of $H_0$ and confirm previous indications that the local universe value of $H_0$ is higher than the early-universe value at $\sim$ $95\%$ confidence. Currently, the Mira-based $H_0$ measurement is still dominated by the statistical uncertainty in the SN Ia peak magnitude. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08423v2-abstract-full').style.display = 'none'; document.getElementById('2312.08423v2-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 11 figures, accepted to ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 963, Issue 2, 2024, id.83, 17 pp., </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/2309.03263">arXiv:2309.03263</a> <span> [<a href="https://arxiv.org/pdf/2309.03263">pdf</a>, <a href="https://arxiv.org/ps/2309.03263">ps</a>, <a href="https://arxiv.org/format/2309.03263">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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"> High-resolution Spectroscopic Metallicities of Milky Way Cepheid Standards and their impact on the Leavitt Law and the Hubble constant </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+A">Anupam Bhardwaj</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=Catanzaro%2C+G">Giovanni Catanzaro</a>, <a href="/search/astro-ph?searchtype=author&query=Trentin%2C+E">Erasmo Trentin</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">Vincenzo Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+M">Marcella Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Ngeow%2C+C">Chow-Choong Ngeow</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=Molinaro%2C+R">Roberto Molinaro</a>, <a href="/search/astro-ph?searchtype=author&query=Singh%2C+H+P">Harinder P. Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Kanbur%2C+S+M">Shashi M. Kanbur</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="2309.03263v1-abstract-short" style="display: inline;"> Milky Way Cepheid variables with accurate {\it Hubble Space Telescope} photometry have been established as standards for primary calibration of the cosmic distance ladder to achieve a percent-level determination of the Hubble constant ($H_0$). These 75 Cepheid standards are the fundamental sample for investigation of possible residual systematics in the local $H_0$ determination due to metallicity… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03263v1-abstract-full').style.display = 'inline'; document.getElementById('2309.03263v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.03263v1-abstract-full" style="display: none;"> Milky Way Cepheid variables with accurate {\it Hubble Space Telescope} photometry have been established as standards for primary calibration of the cosmic distance ladder to achieve a percent-level determination of the Hubble constant ($H_0$). These 75 Cepheid standards are the fundamental sample for investigation of possible residual systematics in the local $H_0$ determination due to metallicity effects on their period-luminosity relations. We obtained new high-resolution ($R\sim81,000$), high signal-to-noise ($S/N\sim50-150$) multi-epoch spectra of 42 out of 75 Cepheid standards using ESPaDOnS instrument at the 3.6-m Canada-France-Hawaii Telescope. Our spectroscopic metallicity measurements are in good agreement with the literature values with systematic differences up to $0.1$ dex due to different metallicity scales. We homogenized and updated the spectroscopic metallicities of all 75 Milky Way Cepheid standards and derived their multiwavelength ($GVIJHK_s$) period-luminosity-metallicity and period-Wesenheit-metallicity relations using the latest {\it Gaia} parallaxes. The metallicity coefficients of these empirically calibrated relations exhibit large uncertainties due to low statistics and a narrow metallicity range ($螖\textrm{[Fe/H]}=0.6$~dex). These metallicity coefficients are up to three times better constrained if we include Cepheids in the Large Magellanic Cloud and range between $-0.21\pm0.07$ and $-0.43\pm0.06$ mag/dex. The updated spectroscopic metallicities of these Milky Way Cepheid standards were used in the Cepheid-Supernovae distance ladder formalism to determine $H_0=72.9~\pm 1.0$\textrm{~km~s$^{-1}$~Mpc$^{-1}$}, suggesting little variation ($\sim 0.1$ ~km~s$^{-1}$~Mpc$^{-1}$) in the local $H_0$ measurements due to different Cepheid metallicity scales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03263v1-abstract-full').style.display = 'none'; document.getElementById('2309.03263v1-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 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">14 pages, 4 figures, Accepted for publication in The Astrophysical Journal Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.10954">arXiv:2308.10954</a> <span> [<a href="https://arxiv.org/pdf/2308.10954">pdf</a>, <a href="https://arxiv.org/format/2308.10954">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 Local Value of H$_0$ </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=Breuval%2C+L">Louise Breuval</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.10954v2-abstract-short" style="display: inline;"> We review the local determination of the Hubble constant, H$_0$, focusing on recent measurements of a distance ladder constructed from geometry, Cepheid variables and Type Ia supernovae (SNe Ia). We explain in some detail the components of the ladder: (1) geometry from Milky Way parallaxes, masers in NGC 4258 and detached eclipsing binaries in the Large Magellanic Cloud; (2) measurements of Cephei… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.10954v2-abstract-full').style.display = 'inline'; document.getElementById('2308.10954v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.10954v2-abstract-full" style="display: none;"> We review the local determination of the Hubble constant, H$_0$, focusing on recent measurements of a distance ladder constructed from geometry, Cepheid variables and Type Ia supernovae (SNe Ia). We explain in some detail the components of the ladder: (1) geometry from Milky Way parallaxes, masers in NGC 4258 and detached eclipsing binaries in the Large Magellanic Cloud; (2) measurements of Cepheids with the Hubble Space Telescope (HST) in these anchors and in the hosts of 42 SNe Ia; and (3) SNe Ia in the Hubble flow. Great attention to negating systematic uncertainties through the use of differential measurements is reviewed. A wide array of tests are discussed. The measurements provide a strong indication of a discrepancy between the local measure of H$_0$ and its value predicted by $螞$CDM theory, calibrated by the cosmic microwave background ($Planck$), a decade-long challenge known as the `Hubble Tension'. We present new measurements with the James Webb Space Telescope of $>$320 Cepheids on both rungs of the distance ladder, in a SN Ia host and the geometric calibrator NGC 4258, showing reduced noise and good agreement with the same as measured with HST. This provides strong evidence that systematic errors in HST Cepheid photometry do not play a significant role in the present Hubble Tension. Future measurements are expected to refine the local determination of the Hubble constant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.10954v2-abstract-full').style.display = 'none'; document.getElementById('2308.10954v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 14 figures. Invited Review for IAU Symposium 376, Richard de Grijs, Patricia Whitelock and Marcio Catelan, eds. Revised version: includes reference to Di Valentino et al. (2021) for Figure 10</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/2306.12858">arXiv:2306.12858</a> <span> [<a href="https://arxiv.org/pdf/2306.12858">pdf</a>, <a href="https://arxiv.org/format/2306.12858">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"> No plateau observed in late-time near-infrared observations of the underluminous Type Ia supernova 2021qvv </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Graur%2C+O">O. Graur</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+E+P">E. Padilla Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+J">J. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Deckers%2C+M">M. Deckers</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=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Karamenhmetoglu%2C+E">E. Karamenhmetoglu</a>, <a href="/search/astro-ph?searchtype=author&query=Stritzinger%2C+M+D">M. D. Stritzinger</a>, <a href="/search/astro-ph?searchtype=author&query=Maguire%2C+K">K. Maguire</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+D+A">D. A. Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Fisher%2C+R">R. Fisher</a>, <a href="/search/astro-ph?searchtype=author&query=Fullard%2C+A+G">A. G. Fullard</a>, <a href="/search/astro-ph?searchtype=author&query=Handberg%2C+R">R. Handberg</a>, <a href="/search/astro-ph?searchtype=author&query=Hiramatsu%2C+D">D. Hiramatsu</a>, <a href="/search/astro-ph?searchtype=author&query=Hosseinzadeh%2C+G">G. Hosseinzadeh</a>, <a href="/search/astro-ph?searchtype=author&query=Kerzendorf%2C+W+E">W. E. Kerzendorf</a>, <a href="/search/astro-ph?searchtype=author&query=McCully%2C+C">C. McCully</a>, <a href="/search/astro-ph?searchtype=author&query=Newsome%2C+M">M. Newsome</a>, <a href="/search/astro-ph?searchtype=author&query=Pellegrino%2C+C">C. Pellegrino</a>, <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">A. Rest</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=Seitenzahl%2C+I+R">I. R. Seitenzahl</a>, <a href="/search/astro-ph?searchtype=author&query=Shara%2C+M+M">M. M. Shara</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+K+J">K. J. Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Terreran%2C+G">G. Terreran</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.12858v2-abstract-short" style="display: inline;"> Near-infrared (NIR) observations of normal Type Ia supernovae (SNe Ia) obtained between 150 to 500 d past maximum light reveal the existence of an extended plateau. Here, we present observations of the underluminous, 1991bg-like SN 2021qvv. Early, ground-based optical and NIR observations show that SN 2021qvv is similar to SN 2006mr, making it one of the dimmest, fastest-evolving 1991bg-like SNe t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.12858v2-abstract-full').style.display = 'inline'; document.getElementById('2306.12858v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.12858v2-abstract-full" style="display: none;"> Near-infrared (NIR) observations of normal Type Ia supernovae (SNe Ia) obtained between 150 to 500 d past maximum light reveal the existence of an extended plateau. Here, we present observations of the underluminous, 1991bg-like SN 2021qvv. Early, ground-based optical and NIR observations show that SN 2021qvv is similar to SN 2006mr, making it one of the dimmest, fastest-evolving 1991bg-like SNe to date. Late-time (170-250 d) Hubble Space Telescope observations of SN 2021qvv reveal no sign of a plateau. An extrapolation of these observations backwards to earlier-phase NIR observations of SN 2006mr suggests the complete absence of a NIR plateau, at least out to 250 d. This absence may be due to a higher ionization state of the ejecta, as predicted by certain sub-Chandrasekhar-mass detonation models, or to the lower temperatures of the ejecta of 1991bg-like SNe, relative to normal SNe Ia, which might preclude their becoming fluorescent and shifting ultraviolet light into the NIR. This suggestion can be tested by acquiring NIR imaging of a sample of 1991bg-like SNe that covers the entire range from slowly-evolving to fast-evolving events ($0.2 \lesssim s_\mathrm{BV} \lesssim 0.6$). A detection of the NIR plateau in slower-evolving, hotter 1991bg-like SNe would provide further evidence that these SNe exist along a continuum with normal SNe Ia. Theoretical progenitor and explosion scenarios would then have to match the observed properties of both SN Ia subtypes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.12858v2-abstract-full').style.display = 'none'; document.getElementById('2306.12858v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS (14 pages, 9 figures)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.10103">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/2304.06695">arXiv:2304.06695</a> <span> [<a href="https://arxiv.org/pdf/2304.06695">pdf</a>, <a href="https://arxiv.org/format/2304.06695">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/accd69">10.3847/1538-4357/accd69 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Gaia Data Release 3 View on the Tip of the Red Giant Branch Luminosity </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=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</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="2304.06695v1-abstract-short" style="display: inline;"> The tip of the red giant branch (TRGB) is a standard candle that can be used to help refine the determination of the Hubble constant. $Gaia$ Data Release 3 (DR3) provides synthetic photometry constructed from low-resolution BP/RP spectra for Milky Way field stars that can be used to directly calibrate the luminosity of the TRGB in the Johnson-Cousins I band, where the TRGB is least sensitive to me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.06695v1-abstract-full').style.display = 'inline'; document.getElementById('2304.06695v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.06695v1-abstract-full" style="display: none;"> The tip of the red giant branch (TRGB) is a standard candle that can be used to help refine the determination of the Hubble constant. $Gaia$ Data Release 3 (DR3) provides synthetic photometry constructed from low-resolution BP/RP spectra for Milky Way field stars that can be used to directly calibrate the luminosity of the TRGB in the Johnson-Cousins I band, where the TRGB is least sensitive to metallicity. We calibrate the TRGB luminosity using a two-dimensional maximum likelihood algorithm with field stars and $Gaia$ synthetic photometry and parallaxes. For a high-contrast and low-contrast break (characterized by the values of the contrast parameter $ R$ or the magnitude of the break $ 尾$), we find $M^{TRGB}_I$ =$-4.02$ and $-3.92$ mag respectively, or a midpoint of $-3.970$ $^{+0.042} _{-0.024}$ (sys) $\pm$ $0.062$ (stat) mag. This measurement improves upon the TRGB measurement from Li et al. (2022), as the higher precision photometry based on $ Gaia $ DR3 allows us to constrain two additional free parameters of the luminosity function. We also investigate the possibility of using $Gaia$ DR3 synthetic photometry to calibrate the TRGB luminosity with $蠅$ Centauri, but find evidence of blending within the inner region for cluster member photometry that precludes accurate calibration with $Gaia$ DR3 photometry. We instead provide an updated TRGB measurement of $m^{TRGB}_I$ = $ 9.82 \pm 0.04$ mag in $蠅$ Centauri using ground-based photometry from the most recent version of the database described in Stetson et al. (2019), which gives $M^{TRGB}_I$ = $-3.97$ $\pm$ $0.04$ (stat) $\pm$ 0.10 (sys) mag when tied to the $Gaia$ EDR3 parallax distance from the consensus of Vasiliev & Baumgardt (2021), Soltis et al. (2021), and Ma铆z Apell谩niz et al. (2022a). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.06695v1-abstract-full').style.display = 'none'; document.getElementById('2304.06695v1-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">17 pages, 10 figures, 3 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 950 83 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.06693">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/2304.00037">arXiv:2304.00037</a> <span> [<a href="https://arxiv.org/pdf/2304.00037">pdf</a>, <a href="https://arxiv.org/format/2304.00037">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/acd3f4">10.3847/1538-4357/acd3f4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A 1.3% distance to M33 from HST Cepheid photometry </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=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=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Konchady%2C+T">Tarini Konchady</a>, <a href="/search/astro-ph?searchtype=author&query=Trahin%2C+B">Boris Trahin</a>, <a href="/search/astro-ph?searchtype=author&query=Durbin%2C+M+J">Meredith J. Durbin</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. 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="2304.00037v1-abstract-short" style="display: inline;"> We present a low-dispersion period-luminosity relation (PL) based on 154 Cepheids in Messier 33 (M33) with Hubble Space Telescope (HST) photometry from the PHATTER survey. Using high-quality ground-based light curves, we recover Cepheid phases and amplitudes for multi-epoch HST data and we perform template fitting to derive intensity-averaged mean magnitudes. HST observations in the SH0ES near-inf… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.00037v1-abstract-full').style.display = 'inline'; document.getElementById('2304.00037v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.00037v1-abstract-full" style="display: none;"> We present a low-dispersion period-luminosity relation (PL) based on 154 Cepheids in Messier 33 (M33) with Hubble Space Telescope (HST) photometry from the PHATTER survey. Using high-quality ground-based light curves, we recover Cepheid phases and amplitudes for multi-epoch HST data and we perform template fitting to derive intensity-averaged mean magnitudes. HST observations in the SH0ES near-infrared Wesenheit system significantly reduce the effect of crowding relative to ground-based data, as seen in the final PL scatter of $蟽$ = 0.11 mag. We adopt the absolute calibration of the PL based on HST observations in the Large Magellanic Cloud (LMC) and a distance derived using late-type detached eclipsing binaries to obtain a distance modulus for M33 of $渭$ = 24.622 $\pm$ 0.030 mag (d = 840 $\pm$ 11 kpc), a best-to-date precision of 1.3%. We find very good agreement with past Cepheid-based measurements. Several TRGB estimates bracket our result while disagreeing with each other. Finally, we show that the flux contribution from star clusters hosting Cepheids in M33 does not impact the distance measurement and we find only 3.7% of the sample is located in (or nearby) young clusters. M33 offers one of the best sites for the cross-calibration of many primary distance indicators. Thus, a precise independent geometric determination of its distance would provide a valuable new anchor to measure the Hubble constant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.00037v1-abstract-full').style.display = 'none'; document.getElementById('2304.00037v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 March, 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 ApJ, comments welcome</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 951 118 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/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/2211.04492">arXiv:2211.04492</a> <span> [<a href="https://arxiv.org/pdf/2211.04492">pdf</a>, <a href="https://arxiv.org/format/2211.04492">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="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> The Hubble Tension and Early Dark Energy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kamionkowski%2C+M">Marc Kamionkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</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="2211.04492v1-abstract-short" style="display: inline;"> Over the past decade, the disparity between the value of the cosmic expansion rate directly determined from measurements of distance and redshift or instead from the standard $螞$CDM cosmological model calibrated by measurements from the early Universe, has grown to a level of significance requiring a solution. Proposed systematic errors are not supported by the breadth of available data (and "unkn… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.04492v1-abstract-full').style.display = 'inline'; document.getElementById('2211.04492v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.04492v1-abstract-full" style="display: none;"> Over the past decade, the disparity between the value of the cosmic expansion rate directly determined from measurements of distance and redshift or instead from the standard $螞$CDM cosmological model calibrated by measurements from the early Universe, has grown to a level of significance requiring a solution. Proposed systematic errors are not supported by the breadth of available data (and "unknown errors" untestable by lack of definition). Simple theoretical explanations for this "Hubble tension" that are consistent with the majority of the data have been surprisingly hard to come by, but in recent years, attention has focused increasingly on models that alter the early or pre-recombination physics of $螞$CDM as the most feasible. Here, we describe the nature of this tension, emphasizing recent developments on the observational side. We then explain why early-Universe solutions are currently favored and the constraints that any such model must satisfy. We discuss one workable example, early dark energy, and describe how it can be tested with future measurements. Given an assortment of more extended recent reviews on specific aspects of the problem, the discussion is intended to be fairly general and understandable to a broad audience. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.04492v1-abstract-full').style.display = 'none'; document.getElementById('2211.04492v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 November, 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">34 pages, 8 figures. Invited Review for Ann. Rev. Nucl. Part. Sci</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.11726">arXiv:2209.11726</a> <span> [<a href="https://arxiv.org/pdf/2209.11726">pdf</a>, <a href="https://arxiv.org/format/2209.11726">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 Physics - Phenomenology">hep-ph</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"> Report of the Topical Group on Cosmic Probes of Fundamental Physics for for Snowmass 2021 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">Rana X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L+A">Luis A. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+K">Ke Fang</a>, <a href="/search/astro-ph?searchtype=author&query=Sathyaprakash%2C+B+S">B. S. Sathyaprakash</a>, <a href="/search/astro-ph?searchtype=author&query=Tollefson%2C+K">Kirsten Tollefson</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+T+R">Tiffany R. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Engel%2C+K">Kristi Engel</a>, <a href="/search/astro-ph?searchtype=author&query=Aboubrahim%2C+A">Amin Aboubrahim</a>, <a href="/search/astro-ph?searchtype=author&query=Akarsu%2C+O">Ozgur Akarsu</a>, <a href="/search/astro-ph?searchtype=author&query=Akrami%2C+Y">Yashar Akrami</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">Roberto Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">Rafael Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Ballardini%2C+M">Mario Ballardini</a>, <a href="/search/astro-ph?searchtype=author&query=Ballmer%2C+S+W">Stefan W. Ballmer</a>, <a href="/search/astro-ph?searchtype=author&query=Bechtol%2C+E">Ellen Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+D">David Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+E">Emanuele Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Birrer%2C+S">Simon Birrer</a>, <a href="/search/astro-ph?searchtype=author&query=Bonilla%2C+A">Alexander Bonilla</a>, <a href="/search/astro-ph?searchtype=author&query=Brito%2C+R">Richard Brito</a>, <a href="/search/astro-ph?searchtype=author&query=Bustamante%2C+M">Mauricio Bustamante</a>, <a href="/search/astro-ph?searchtype=author&query=Caldwell%2C+R">Robert Caldwell</a>, <a href="/search/astro-ph?searchtype=author&query=Cardoso%2C+V">Vitor Cardoso</a>, <a href="/search/astro-ph?searchtype=author&query=Chakrabarti%2C+S">Sukanya Chakrabarti</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+T+Y">Thomas Y. Chen</a> , et al. (96 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="2209.11726v1-abstract-short" style="display: inline;"> Cosmic Probes of Fundamental Physics take two primary forms: Very high energy particles (cosmic rays, neutrinos, and gamma rays) and gravitational waves. Already today, these probes give access to fundamental physics not available by any other means, helping elucidate the underlying theory that completes the Standard Model. The last decade has witnessed a revolution of exciting discoveries such as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.11726v1-abstract-full').style.display = 'inline'; document.getElementById('2209.11726v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.11726v1-abstract-full" style="display: none;"> Cosmic Probes of Fundamental Physics take two primary forms: Very high energy particles (cosmic rays, neutrinos, and gamma rays) and gravitational waves. Already today, these probes give access to fundamental physics not available by any other means, helping elucidate the underlying theory that completes the Standard Model. The last decade has witnessed a revolution of exciting discoveries such as the detection of high-energy neutrinos and gravitational waves. The scope for major developments in the next decades is dramatic, as we detail in this report. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.11726v1-abstract-full').style.display = 'none'; document.getElementById('2209.11726v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">Report of theTopical Group on Cosmic Probes of Fundamental Physics, for the U.S. decadal Particle Physics Planning Exercise (Snowmass 2021)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.09101">arXiv:2209.09101</a> <span> [<a href="https://arxiv.org/pdf/2209.09101">pdf</a>, <a href="https://arxiv.org/format/2209.09101">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.3847/2041-8213/ac9b27">10.3847/2041-8213/ac9b27 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A First Look at Cepheids in a SN Ia Host with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Wenlong Yuan</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=Macri%2C+L+M">Lucas M. Macri</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="2209.09101v1-abstract-short" style="display: inline;"> We report the first look at extragalactic Cepheid variables with the James Webb Space Telescope, obtained from a serendipitous (to this purpose) observation of NGC 1365, host of an SN Ia (SN 2012fr), a calibration path used to measure the Hubble constant. As expected, the high-resolution observations with NIRCam through F200W show better source separation from line-of-sight companions than HST ima… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.09101v1-abstract-full').style.display = 'inline'; document.getElementById('2209.09101v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.09101v1-abstract-full" style="display: none;"> We report the first look at extragalactic Cepheid variables with the James Webb Space Telescope, obtained from a serendipitous (to this purpose) observation of NGC 1365, host of an SN Ia (SN 2012fr), a calibration path used to measure the Hubble constant. As expected, the high-resolution observations with NIRCam through F200W show better source separation from line-of-sight companions than HST images at similar near-infrared wavelengths, the spectral region that has been used to mitigate the impact of host dust on distance measurements. Using the standard star P330E as a zeropoint and PSF reference, we photometered 31 previously-known Cepheids in the JWST field, spanning 1.15 < log P < 1.75 including 24 Cepheids in the longer period interval of 1.35 < log P < 1.75. We compared the resultant Period-Luminosity relations to that of 49 Cepheids in the full period range including 38 in the longer period range observed with WFC3/IR on HST and transformed to the JWST photometric system (F200W, Vega). The P-L relations measured with the two space telescopes are in good agreement, with intercepts (at log P=1) of 25.74+/-0.04 and 25.72+\-0.05 for HST and JWST, respectively. Our baseline result comes from the longer period range where the Cepheids have higher signal-to-noise ratios where we find 25.75+\-0.05 and 25.75+\-0.06 mag for HST and JWST, respectively. We find good consistency between this first JWST measurement and HST, and no evidence that HST Cepheid photometry is "biased bright" at the ~0.2 mag level that would be needed to mitigate the Hubble Tension, though comparisons from more SN hosts are warranted and anticipated. We expect future JWST observations to surpass these in quality as they will be optimized for measuring Cepheids. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.09101v1-abstract-full').style.display = 'none'; document.getElementById('2209.09101v1-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 4 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.02546">arXiv:2209.02546</a> <span> [<a href="https://arxiv.org/pdf/2209.02546">pdf</a>, <a href="https://arxiv.org/format/2209.02546">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/10.1051/0004-6361/202244893">10.1051/0004-6361/202244893 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An updated measurement of the Hubble constant from near-infrared observations of Type Ia supernovae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">Llu铆s Galbany</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=Riess%2C+A+G">Adam G. Riess</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller-Bravo%2C+T+E">Tom谩s E. M眉ller-Bravo</a>, <a href="/search/astro-ph?searchtype=author&query=Dhawan%2C+S">Suhail Dhawan</a>, <a href="/search/astro-ph?searchtype=author&query=Phan%2C+K">Kim Phan</a>, <a href="/search/astro-ph?searchtype=author&query=Stritzinger%2C+M">Maximillian Stritzinger</a>, <a href="/search/astro-ph?searchtype=author&query=Karamehmetoglu%2C+E">Emir Karamehmetoglu</a>, <a href="/search/astro-ph?searchtype=author&query=Leibundgut%2C+B">Bruno Leibundgut</a>, <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+E">Erik Peterson</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=Johansson%2C+J">Joel Johansson</a>, <a href="/search/astro-ph?searchtype=author&query=Maguire%2C+K">Kate Maguire</a>, <a href="/search/astro-ph?searchtype=author&query=Jha%2C+S+W">Saurabh W. Jha</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="2209.02546v2-abstract-short" style="display: inline;"> We present a measurement of the Hubble constant ($H_0$) using type Ia supernova (SNe Ia) in the near-infrared (NIR) from the recently updated sample of SNe Ia in nearby galaxies with distances measured via Cepheid period-luminosity relations by the SHOES project. We collect public near-infrared photometry of up to 19 calibrator SNe Ia and further 57 SNe Ia in the Hubble flow ($z>0.01$), and direct… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.02546v2-abstract-full').style.display = 'inline'; document.getElementById('2209.02546v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.02546v2-abstract-full" style="display: none;"> We present a measurement of the Hubble constant ($H_0$) using type Ia supernova (SNe Ia) in the near-infrared (NIR) from the recently updated sample of SNe Ia in nearby galaxies with distances measured via Cepheid period-luminosity relations by the SHOES project. We collect public near-infrared photometry of up to 19 calibrator SNe Ia and further 57 SNe Ia in the Hubble flow ($z>0.01$), and directly measure their peak magnitudes in the $J$ and $H$ band by Gaussian processes and spline interpolation. Calibrator peak magnitudes together with Cepheid-based distances are used to estimate the average absolute magnitude in each band, while Hubble-flow SNe are used to constrain the zero-point intercept of the magnitude-redshift relation. Our baseline result of $H_0$ is $72.3\pm1.4$ (stat) $\pm1.4$ (syst) km s$^{-1}$ Mpc$^{-1}$ in the $J$ band and $72.3\pm1.3$ (stat) $\pm1.4$ (syst) km s$^{-1}$ Mpc$^{-1}$ in the $H$ band, where the systematic uncertainties include the standard deviation of up to 21 variations of the analysis, the 0.7\% distance scale systematic from SHOES Cepheid anchors, a photometric zeropoint systematic, and a cosmic variance systematic. Our final measurement represents a measurement with a precision of 2.8\% in both bands. The variant with the largest change in $H_0$ is when limiting the sample to SNe from CSP and CfA programmes, noteworthy because these are the best calibrated, yielding $H_0\sim75$ km s$^{-1}$ Mpc$^{-1}$ in both bands. We demonstrate stretch and reddening corrections are still useful in the NIR to standardize SN Ia NIR peak magnitudes. Based on our results, in order to improve the precision of the $H_0$ measurement with SNe Ia in the NIR in the future, we would need to increase the number of calibrator SNe Ia, be able to extend the Hubble-Lema卯tre diagram to higher-z, and include standardization procedures to help reducing the NIR intrinsic scatter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.02546v2-abstract-full').style.display = 'none'; document.getElementById('2209.02546v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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, 8 figures. Accepted in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 679, A95 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.01045">arXiv:2208.01045</a> <span> [<a href="https://arxiv.org/pdf/2208.01045">pdf</a>, <a href="https://arxiv.org/format/2208.01045">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/ac8f24">10.3847/1538-4357/ac8f24 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cluster Cepheids with High Precision Gaia Parallaxes, Low Zeropoint Uncertainties, and Hubble Space Telescope Photometry </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=Breuval%2C+L">Louise Breuval</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=~Macri%2C+L+M">Lucas M. ~Macri</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">Tristan Cantat-Gaudin</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=Reyes%2C+M+C">Mauricio Cruz Reyes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.01045v1-abstract-short" style="display: inline;"> We present HST photometry of 17 Cepheids in open clusters and their mean parallaxes from Gaia EDR3. These parallaxes are more precise than those from individual Cepheids (G<8 mag) previously used to measure the Hubble constant because they are derived from an average of >300 stars per cluster. Cluster parallaxes also have smaller systematic uncertainty because their stars lie in the range (G>13 ma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.01045v1-abstract-full').style.display = 'inline'; document.getElementById('2208.01045v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.01045v1-abstract-full" style="display: none;"> We present HST photometry of 17 Cepheids in open clusters and their mean parallaxes from Gaia EDR3. These parallaxes are more precise than those from individual Cepheids (G<8 mag) previously used to measure the Hubble constant because they are derived from an average of >300 stars per cluster. Cluster parallaxes also have smaller systematic uncertainty because their stars lie in the range (G>13 mag) where the Gaia parallax calibration is most comprehensive. Cepheid photometry employed in the period--luminosity relation was measured using the same instrument(WFC3) and filters(F555W,F814W,F160W) as extragalactic Cepheids in SNIa hosts. We find no evidence of residual parallax offset in this magnitude range, zp=-3+/-4 muas, consistent with Lindegren:2021b and most studies. The Cepheid luminosity (P=10d, solar-metallicity) in the HST near-infrared, Wesenheit system derived from the cluster sample is M_{H,1}^W=-5.902+/-0.025 and -5.890+/-0.018 mag with or without simultaneous determination of a parallax offset, respectively. These results are similar to measurements from field Cepheids, confirming the accuracy of the Gaia parallaxes over a broad range of magnitudes. The SH0ES distance ladder calibrated solely from this sample gives H_0=72.8+/-1.3 and H_0=73.2+/-1.1 km/s/Mpc with or without offset marginalization; combined with all anchors we find H_0=73.01+/-0.99 and 73.15+/-0.97, respectively, a 5% or 7% reduction in the uncertainty and a 5.3 sigma Hubble Tension relative to Planck+LambdaCDM. It appears increasingly difficult to reconcile two of the best measured cosmic scales, parallaxes from Gaia and the angular size of the acoustic scale of the CMB, using the simplest form of LambdaCDM to join the two. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.01045v1-abstract-full').style.display = 'none'; document.getElementById('2208.01045v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 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/2205.06280">arXiv:2205.06280</a> <span> [<a href="https://arxiv.org/pdf/2205.06280">pdf</a>, <a href="https://arxiv.org/format/2205.06280">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </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/ac97e2">10.3847/1538-4357/ac97e2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Improved Calibration of the Wavelength Dependence of Metallicity on the Cepheid Leavitt law </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=Kervella%2C+P">Pierre Kervella</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=Romaniello%2C+M">Martino Romaniello</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.06280v2-abstract-short" style="display: inline;"> The Cepheid period-luminosity (PL) relation (or Leavitt law) has served as the first rung of the most widely used extragalactic distance ladder and is central to the determination of the local value of the Hubble constant ($H_0$). We investigate the influence of metallicity on Cepheid brightness, a term that significantly improves the overall fit of the distance ladder, to better define its wavele… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.06280v2-abstract-full').style.display = 'inline'; document.getElementById('2205.06280v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.06280v2-abstract-full" style="display: none;"> The Cepheid period-luminosity (PL) relation (or Leavitt law) has served as the first rung of the most widely used extragalactic distance ladder and is central to the determination of the local value of the Hubble constant ($H_0$). We investigate the influence of metallicity on Cepheid brightness, a term that significantly improves the overall fit of the distance ladder, to better define its wavelength dependence. To this aim, we compare the PL relations obtained for three Cepheid samples having distinct chemical composition (in the Milky Way and Magellanic Clouds) and focusing on the use of improved and recent data while covering a metallicity range of about 1 dex. We estimate the metallicity effect (hereafter $纬$) in 15 filters from mid-IR to optical wavelengths, including five Wesenheit indices, and we derive a significant metallicity term in all filters, in agreement with recent empirical studies and models, in the sense of metal-rich Cepheids being brighter than metal-poor ones. We describe the contribution of various systematic effects in the determination of the $纬$ term. We find no evidence of $纬$ changing over the wavelength range $0.5-4.5 \, \rm 渭m$, indicating that the main influence of metallicity on Cepheids is in their luminosity rather than color. Finally, we identify factors that sharpen the empirical constraints on the metallicity term over past studies, including corrections for the depth of the Magellanic Clouds, better-calibrated Cepheid photometry, improved Milky Way extinction estimates, and revised and expanded metallicity measurements in the LMC. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.06280v2-abstract-full').style.display = 'none'; document.getElementById('2205.06280v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 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/2204.13553">arXiv:2204.13553</a> <span> [<a href="https://arxiv.org/pdf/2204.13553">pdf</a>, <a href="https://arxiv.org/format/2204.13553">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/stad1652">10.1093/mnras/stad1652 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Synthetic Roman Space Telescope High-Latitude Time-Domain Survey: Supernovae in the Deep Field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+K+X">Kevin X. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Troxel%2C+M+A">M. A. Troxel</a>, <a href="/search/astro-ph?searchtype=author&query=Rodney%2C+S+A">Steven A. Rodney</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">Brodie Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Duff%2C+C">Caleb Duff</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=Foley%2C+R+J">Ryan J. Foley</a>, <a href="/search/astro-ph?searchtype=author&query=Hounsell%2C+R">Rebekah Hounsell</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=Jones%2C+D+O">David O. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+B+A">Bhavin A. Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+H">Heyang Long</a>, <a href="/search/astro-ph?searchtype=author&query=Macias%2C+P">Phillip Macias</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=Rose%2C+B+M">Benjamin M. Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Yamamoto%2C+M">Masaya Yamamoto</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.13553v2-abstract-short" style="display: inline;"> NASA will launch the Nancy Grace Roman Space Telescope (Roman) in the second half of this decade, which will allow for a generation-defining measurement of dark energy through multiple probes, including Type Ia supernovae (SNe Ia). To improve decisions on survey strategy, we have created the first simulations of realistic Roman images that include artificial SNe Ia injected as point sources in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.13553v2-abstract-full').style.display = 'inline'; document.getElementById('2204.13553v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.13553v2-abstract-full" style="display: none;"> NASA will launch the Nancy Grace Roman Space Telescope (Roman) in the second half of this decade, which will allow for a generation-defining measurement of dark energy through multiple probes, including Type Ia supernovae (SNe Ia). To improve decisions on survey strategy, we have created the first simulations of realistic Roman images that include artificial SNe Ia injected as point sources in the images. Our analysis combines work done on Roman simulations for weak gravitational lensing studies as well as catalog-level simulations of SN samples. We have created a time series of images over two years containing $\sim$ 1,050 SNe Ia, covering a 1 square degree subarea of a planned 5 square degree deep survey. We have released these images publicly for community use along with input catalogs of all injected sources. We create secondary products from these images by generating coadded images and demonstrating recovery of transient sources using image subtraction. We perform first-use analyses on these images in order to measure galaxy-detection efficiency, point source-detection efficiency, and host-galaxy association biases. The simulated images can be found here: https://roman.ipac.caltech.edu/sims/SN_Survey_Image_sim.html. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.13553v2-abstract-full').style.display = 'none'; document.getElementById('2204.13553v2-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 12 figures. Submitted to MNRAS. For simulated images see https://roman.ipac.caltech.edu/sims/SN_Survey_Image_sim.html</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.10866">arXiv:2204.10866</a> <span> [<a href="https://arxiv.org/pdf/2204.10866">pdf</a>, <a href="https://arxiv.org/format/2204.10866">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/ac80bd">10.3847/1538-4357/ac80bd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of the Hubble Constant with a Two Rung Distance Ladder: Two Out of Three Ain't Bad </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=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=Yuan%2C+W">Wenlong Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Bernal%2C+J+L">Jos茅 Luis Bernal</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">Dillon Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Cassertano%2C+S">Stefano Cassertano</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=Macri%2C+L">Lucas Macri</a>, <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+E">Erik Peterson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.10866v1-abstract-short" style="display: inline;"> The three rung distance ladder, which calibrates Type Ia supernovae through stellar distances linked to geometric measurements, provides the highest precision direct measurement of the Hubble constant. In light of the Hubble tension, it is important to test the individual components of the distance ladder. For this purpose, we report a measurement of the Hubble constant from 35 extragalactic Cephe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.10866v1-abstract-full').style.display = 'inline'; document.getElementById('2204.10866v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.10866v1-abstract-full" style="display: none;"> The three rung distance ladder, which calibrates Type Ia supernovae through stellar distances linked to geometric measurements, provides the highest precision direct measurement of the Hubble constant. In light of the Hubble tension, it is important to test the individual components of the distance ladder. For this purpose, we report a measurement of the Hubble constant from 35 extragalactic Cepheid hosts measured by the SH0ES team, using their distances and redshifts at cz < 3300 km /s , instead of any, more distant Type Ia supernovae, to measure the Hubble flow. The Cepheid distances are calibrated geometrically in the Milky Way, NGC 4258, and the Large Magellanic Cloud. Peculiar velocities are a significant source of systematic uncertainty at z $\sim$ 0.01, and we present a formalism for both mitigating and quantifying their effects, making use of external reconstructions of the density and velocity fields in the nearby universe. We identify a significant source of uncertainty originating from different assumptions about the selection criteria of this sample, whether distance or redshift limited, as it was assembled over three decades. Modeling these assumptions yields central values ranging from H0 = 71.8 to 77.0 km/s/Mpc. Combining the four best fitting selection models yields H0 = 73.1 (+2.6/-2.3) km/s/Mpc as a fiducial result, at $2.6蟽$ tension with Planck. While Type Ia supernovae are essential for a precise measurement of H0, unknown systematics in these supernovae are unlikely to be the source of the Hubble tension <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.10866v1-abstract-full').style.display = 'none'; document.getElementById('2204.10866v1-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 Pages, 11 Figures, 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/2203.08974">arXiv:2203.08974</a> <span> [<a href="https://arxiv.org/pdf/2203.08974">pdf</a>, <a href="https://arxiv.org/format/2203.08974">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/stac1661">10.1093/mnras/stac1661 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A 5% measurement of the Hubble constant from Type II supernovae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Jaeger%2C+T">T. de Jaeger</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</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=Stahl%2C+B+E">B. E. Stahl</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">B. J. Shappee</a>, <a href="/search/astro-ph?searchtype=author&query=Filippenko%2C+A+V">A. V. Filippenko</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W">W. Zheng</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.08974v2-abstract-short" style="display: inline;"> The most stringent local measurement of the Hubble-Lema卯tre constant from Cepheid-calibrated Type Ia supernovae (SNe~Ia) differs from the value inferred via the cosmic microwave background radiation ({\it Planck}$+螞$CDM) by $\sim 5蟽$. This so-called "Hubble tension" has been confirmed by other independent methods, and thus does not appear to be a possible consequence of systematic errors. Here, we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.08974v2-abstract-full').style.display = 'inline'; document.getElementById('2203.08974v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.08974v2-abstract-full" style="display: none;"> The most stringent local measurement of the Hubble-Lema卯tre constant from Cepheid-calibrated Type Ia supernovae (SNe~Ia) differs from the value inferred via the cosmic microwave background radiation ({\it Planck}$+螞$CDM) by $\sim 5蟽$. This so-called "Hubble tension" has been confirmed by other independent methods, and thus does not appear to be a possible consequence of systematic errors. Here, we continue upon our prior work of using Type II supernovae to provide another, largely-independent method to measure the Hubble-Lema卯tre constant. From 13 SNe~II with geometric, Cepheid, or tip of the red giant branch (TRGB) host-galaxy distance measurements, we derive H$_0= 75.4^{+3.8}_{-3.7}$\,km\,s$^{-1}$\,Mpc$^{-1}$ (statistical errors only), consistent with the local measurement but in disagreement by $\sim 2.0蟽$ with the {\it Planck}$+螞$CDM value. Using only Cepheids ($N=7$), we find H$_0 = 77.6^{+5.2}_{-4.8}$\,km\,s$^{-1}$\,Mpc$^{-1}$, while using only TRGB ($N=5$), we derive H$_0 = 73.1^{+5.7}_{-5.3}$\,km\,s$^{-1}$\,Mpc$^{-1}$. Via 13 variants of our dataset, we derive a systematic uncertainty estimate of 1.5\,km\,s$^{-1}$\,Mpc$^{-1}$. The median value derived from these variants differs by just 0.3\,km\,s$^{-1}$\,Mpc$^{-1}$ from that produced by our fiducial model. Because we only replace SNe~Ia with SNe~II -- and we do not find statistically significant difference between the Cepheid and TRGB H$_0$ measurements -- our work reveals no indication that SNe~Ia or Cepheids could be the sources of the "H$_0$ tension." We caution, however, that our conclusions rest upon a modest calibrator sample; as this sample grows in the future, our results should be verified. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.08974v2-abstract-full').style.display = 'none'; document.getElementById('2203.08974v2-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 4 figures, 2 tables. Accepted for publication by MNRAS. arXiv admin note: text overlap with arXiv:2006.03412</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.06681">arXiv:2203.06681</a> <span> [<a href="https://arxiv.org/pdf/2203.06681">pdf</a>, <a href="https://arxiv.org/format/2203.06681">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac51db">10.3847/1538-4357/ac51db <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Absolute Calibration of Cepheid Period-Luminosity Relations in NGC 4258 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Riess%2C+A+G">Adam G. Riess</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+T+G">Thomas G. Brink</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</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=Hoffmann%2C+S+L">Samantha L. Hoffmann</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=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="2203.06681v1-abstract-short" style="display: inline;"> NGC 4258 is one of the most important anchors for calibrating the Cepheid period--luminosity relations (PLRs) owing to its accurate distance measured from water maser motions. We expand on previous efforts and carry out a new Cepheid search in this system using the Hubble Space Telescope (HST). We discover and measure a sample of 669 Cepheids in four new and two archival NGC 4258 fields, doubling… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06681v1-abstract-full').style.display = 'inline'; document.getElementById('2203.06681v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.06681v1-abstract-full" style="display: none;"> NGC 4258 is one of the most important anchors for calibrating the Cepheid period--luminosity relations (PLRs) owing to its accurate distance measured from water maser motions. We expand on previous efforts and carry out a new Cepheid search in this system using the Hubble Space Telescope (HST). We discover and measure a sample of 669 Cepheids in four new and two archival NGC 4258 fields, doubling the number of known Cepheids in this galaxy and obtaining an absolute calibration of their optical PLRs. We determine a Wesenheit PLR of $-2.574(\pm0.034) -3.294(\pm0.042) \log P$, consistent with an independent Large Magellanic Cloud (LMC) calibration at the level of $0.032\pm0.044$~mag in its zeropoint, after accounting for a metallicity dependence of $-0.20\pm0.05$~mag\,dex$^{-1}$ (Riess et al. 2006). Our determination of the PLR slope also agrees with the LMC-based value within their uncertainties. We attempt to characterize the metallicity effect of Cepheid PLRs using only the NGC 4258 sample, but a relatively narrow span of abundances limits our sensitivity and yields a Wesenheit zero-point dependence of $-0.07 \pm 0.21$ mag\,dex$^{-1}$. The Cepheid measurements presented in this study have been used as part of the data to derive the Hubble constant in a companion paper by the SH0ES team. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06681v1-abstract-full').style.display = 'none'; document.getElementById('2203.06681v1-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ. 13 pages, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.06142">arXiv:2203.06142</a> <span> [<a href="https://arxiv.org/pdf/2203.06142">pdf</a>, <a href="https://arxiv.org/format/2203.06142">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 Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.jheap.2022.04.002">10.1016/j.jheap.2022.04.002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmology Intertwined: A Review of the Particle Physics, Astrophysics, and Cosmology Associated with the Cosmological Tensions and Anomalies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+E">Elcio Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Abell%C3%A1n%2C+G+F">Guillermo Franco Abell谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Aboubrahim%2C+A">Amin Aboubrahim</a>, <a href="/search/astro-ph?searchtype=author&query=Agnello%2C+A">Adriano Agnello</a>, <a href="/search/astro-ph?searchtype=author&query=Akarsu%2C+O">Ozgur Akarsu</a>, <a href="/search/astro-ph?searchtype=author&query=Akrami%2C+Y">Yashar Akrami</a>, <a href="/search/astro-ph?searchtype=author&query=Alestas%2C+G">George Alestas</a>, <a href="/search/astro-ph?searchtype=author&query=Aloni%2C+D">Daniel Aloni</a>, <a href="/search/astro-ph?searchtype=author&query=Amendola%2C+L">Luca Amendola</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L+A">Luis A. Anchordoqui</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=Arendse%2C+N">Nikki Arendse</a>, <a href="/search/astro-ph?searchtype=author&query=Asgari%2C+M">Marika Asgari</a>, <a href="/search/astro-ph?searchtype=author&query=Ballardini%2C+M">Mario Ballardini</a>, <a href="/search/astro-ph?searchtype=author&query=Barger%2C+V">Vernon Barger</a>, <a href="/search/astro-ph?searchtype=author&query=Basilakos%2C+S">Spyros Basilakos</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+C">Ronaldo C. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Battistelli%2C+E+S">Elia S. Battistelli</a>, <a href="/search/astro-ph?searchtype=author&query=Battye%2C+R">Richard Battye</a>, <a href="/search/astro-ph?searchtype=author&query=Benetti%2C+M">Micol Benetti</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+D">David Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berlin%2C+A">Asher Berlin</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+E">Emanuele Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Bidenko%2C+B">Bohdan Bidenko</a> , et al. (178 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.06142v3-abstract-short" style="display: inline;"> In this paper we will list a few important goals that need to be addressed in the next decade, also taking into account the current discordances between the different cosmological probes, such as the disagreement in the value of the Hubble constant $H_0$, the $蟽_8$--$S_8$ tension, and other less statistically significant anomalies. While these discordances can still be in part the result of system… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06142v3-abstract-full').style.display = 'inline'; document.getElementById('2203.06142v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.06142v3-abstract-full" style="display: none;"> In this paper we will list a few important goals that need to be addressed in the next decade, also taking into account the current discordances between the different cosmological probes, such as the disagreement in the value of the Hubble constant $H_0$, the $蟽_8$--$S_8$ tension, and other less statistically significant anomalies. While these discordances can still be in part the result of systematic errors, their persistence after several years of accurate analysis strongly hints at cracks in the standard cosmological scenario and the necessity for new physics or generalisations beyond the standard model. In this paper, we focus on the $5.0\,蟽$ tension between the {\it Planck} CMB estimate of the Hubble constant $H_0$ and the SH0ES collaboration measurements. After showing the $H_0$ evaluations made from different teams using different methods and geometric calibrations, we list a few interesting new physics models that could alleviate this tension and discuss how the next decade's experiments will be crucial. Moreover, we focus on the tension of the {\it Planck} CMB data with weak lensing measurements and redshift surveys, about the value of the matter energy density $惟_m$, and the amplitude or rate of the growth of structure ($蟽_8,f蟽_8$). We list a few interesting models proposed for alleviating this tension, and we discuss the importance of trying to fit a full array of data with a single model and not just one parameter at a time. Additionally, we present a wide range of other less discussed anomalies at a statistical significance level lower than the $H_0$--$S_8$ tensions which may also constitute hints towards new physics, and we discuss possible generic theoretical approaches that can collectively explain the non-standard nature of these signals.[Abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06142v3-abstract-full').style.display = 'none'; document.getElementById('2203.06142v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Contribution to Snowmass 2021. 224 pages, 27 figures. Accepted for publication in JHEAp</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. High En. Astrophys. 2204, 002 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.11110">arXiv:2202.11110</a> <span> [<a href="https://arxiv.org/pdf/2202.11110">pdf</a>, <a href="https://arxiv.org/format/2202.11110">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/ac7559">10.3847/1538-4357/ac7559 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Maximum Likelihood Calibration of the Tip of the Red Giant Branch Luminosity from High Latitude Field Giants using Gaia Early Data Release 3 Parallaxes </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=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</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="2202.11110v3-abstract-short" style="display: inline;"> The calibration of the tip of the red giant branch (TRGB) in the $I$-band has a direct role in determinations of the Hubble constant, a subject of recent interest due to the discrepancy between direct and indirect estimates of its value. We present a maximum likelihood (ML) method designed to obtain an independent calibration of the brightness of TRGB using $Gaia$ parallaxes from the Early Data Re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.11110v3-abstract-full').style.display = 'inline'; document.getElementById('2202.11110v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.11110v3-abstract-full" style="display: none;"> The calibration of the tip of the red giant branch (TRGB) in the $I$-band has a direct role in determinations of the Hubble constant, a subject of recent interest due to the discrepancy between direct and indirect estimates of its value. We present a maximum likelihood (ML) method designed to obtain an independent calibration of the brightness of TRGB using $Gaia$ parallaxes from the Early Data Release 3 (EDR3) of Milky Way field Giants at high Galactic latitude. We adopt simple parameterizations for the Milky Way stellar luminosity function and density law and and optimize the likelihood of the observed sample as a function of those parameters. Using parameters to partially constrain the luminosity function from other galaxies similar to the Milky Way for which high quality TRGB data are available, we find values of the TRGB magnitude of $ M_I^{TRGB} = -3.91 \pm 0.05 $ (stat) $ \pm 0.09 $ (sys) mag, where the systematic uncertainty covers the range of shape parameters found in our Milky Way sample and in reference galaxies. While APASS Data Release 9 all-sky photometry is insufficient to provide a reliable constraint on the shape of the Milky Way luminosity function, we estimate that the photometry from $Gaia$ Data Release 3 (mid-2022) will allow better constraints on the shape, and lower statistical uncertainties on the tip by a factor of 3. With expected releases of improved parallax measurements from $Gaia$, the method of calibrating the TRGB luminosity from field Giants is expected to reach $\sim$ 0.01 mag uncertainty, which is an important step toward a precise TRGB-based determination of the Hubble constant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.11110v3-abstract-full').style.display = 'none'; document.getElementById('2202.11110v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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, 6 figures, 4 tables, Accepted by ApJ, This version contains changes from fixing a filter transformation</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.04077">arXiv:2202.04077</a> <span> [<a href="https://arxiv.org/pdf/2202.04077">pdf</a>, <a href="https://arxiv.org/format/2202.04077">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/ac8e04">10.3847/1538-4357/ac8e04 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pantheon+ Analysis: Cosmological Constraints </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">Dillon Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</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=Zuntz%2C+J">Joe Zuntz</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">Rick Kessler</a>, <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=Hinton%2C+S">Samuel Hinton</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D">David Jones</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=Peterson%2C+E+R">Erik R. Peterson</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>, <a href="/search/astro-ph?searchtype=author&query=Ali%2C+N">Noor Ali</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">Patrick Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Charvu%2C+P">Pranav Charvu</a>, <a href="/search/astro-ph?searchtype=author&query=Dwomoh%2C+A">Arianna Dwomoh</a>, <a href="/search/astro-ph?searchtype=author&query=Palmese%2C+A">Antonella Palmese</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">Helen Qu</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=Stubbs%2C+C+W">Christopher W. Stubbs</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">Maria Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Wood%2C+C+M">Charlotte M. Wood</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+P+J">Peter J. Brown</a> , et al. (21 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.04077v2-abstract-short" style="display: inline;"> We present constraints on cosmological parameters from the Pantheon+ analysis of 1701 light curves of 1550 distinct Type Ia supernovae (SNe Ia) ranging in redshift from $z=0.001$ to 2.26. This work features an increased sample size, increased redshift span, and improved treatment of systematic uncertainties in comparison to the original Pantheon analysis and results in a factor of two improvement… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.04077v2-abstract-full').style.display = 'inline'; document.getElementById('2202.04077v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.04077v2-abstract-full" style="display: none;"> We present constraints on cosmological parameters from the Pantheon+ analysis of 1701 light curves of 1550 distinct Type Ia supernovae (SNe Ia) ranging in redshift from $z=0.001$ to 2.26. This work features an increased sample size, increased redshift span, and improved treatment of systematic uncertainties in comparison to the original Pantheon analysis and results in a factor of two improvement in cosmological constraining power. For a Flat$螞$CDM model, we find $惟_M=0.334\pm0.018$ from SNe Ia alone. For a Flat$w_0$CDM model, we measure $w_0=-0.90\pm0.14$ from SNe Ia alone, H$_0=73.5\pm1.1$ km s$^{-1}$ Mpc$^{-1}$ when including the Cepheid host distances and covariance (SH0ES), and $w_0=-0.978^{+0.024}_{-0.031}$ when combining the SN likelihood with constraints from the cosmic microwave background (CMB) and baryon acoustic oscillations (BAO); both $w_0$ values are consistent with a cosmological constant. We also present the most precise measurements to date on the evolution of dark energy in a Flat$w_0w_a$CDM universe, and measure $w_a=-0.1^{+0.9}_{-2.0}$ from Pantheon+ alone, H$_0=73.3\pm1.1$ km s$^{-1}$ Mpc$^{-1}$ when including SH0ES, and $w_a=-0.65^{+0.28}_{-0.32}$ when combining Pantheon+ with CMB and BAO data. Finally, we find that systematic uncertainties in the use of SNe Ia along the distance ladder comprise less than one third of the total uncertainty in the measurement of H$_0$ and cannot explain the present "Hubble tension" between local measurements and early-Universe predictions from the cosmological model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.04077v2-abstract-full').style.display = 'none'; document.getElementById('2202.04077v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">34 Pages, 16 Figures, 7 Tables. Published in ApJ. Comments welcome. Papers and data release here: https://pantheonplussh0es.github.io</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 938 110 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.07801">arXiv:2201.07801</a> <span> [<a href="https://arxiv.org/pdf/2201.07801">pdf</a>, <a href="https://arxiv.org/format/2201.07801">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/10.3847/1538-4357/ac755b">10.3847/1538-4357/ac755b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmological Results from the RAISIN Survey: Using Type Ia Supernovae in the Near Infrared as a Novel Path to Measure the Dark Energy Equation of State </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+O">D. O. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Mandel%2C+K+S">K. S. Mandel</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=Thorp%2C+S">S. Thorp</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=Avelino%2C+A">A. Avelino</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+C">C. Burns</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=Pan%2C+Y+-">Y. -C. Pan</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=Siebert%2C+M+R">M. R. Siebert</a>, <a href="/search/astro-ph?searchtype=author&query=Chornock%2C+R">R. Chornock</a>, <a href="/search/astro-ph?searchtype=author&query=Freedman%2C+W+L">W. L. Freedman</a>, <a href="/search/astro-ph?searchtype=author&query=Friedman%2C+A">A. Friedman</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=Hsiao%2C+E">E. Hsiao</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Marion%2C+G+H">G. H. Marion</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=Nugent%2C+P+E">P. E. Nugent</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M+M">M. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">A. Rest</a>, <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">A. G. Riess</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.07801v2-abstract-short" style="display: inline;"> Type Ia supernovae (SNe Ia) are more precise standardizable candles when measured in the near-infrared (NIR) than in the optical. With this motivation, from 2012-2017 we embarked on the RAISIN program with the Hubble Space Telescope (HST) to obtain rest-frame NIR light curves for a cosmologically distant sample of 37 SN Ia ($0.2 \lesssim z \lesssim 0.6$) discovered by Pan-STARRS and the Dark Energ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.07801v2-abstract-full').style.display = 'inline'; document.getElementById('2201.07801v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.07801v2-abstract-full" style="display: none;"> Type Ia supernovae (SNe Ia) are more precise standardizable candles when measured in the near-infrared (NIR) than in the optical. With this motivation, from 2012-2017 we embarked on the RAISIN program with the Hubble Space Telescope (HST) to obtain rest-frame NIR light curves for a cosmologically distant sample of 37 SN Ia ($0.2 \lesssim z \lesssim 0.6$) discovered by Pan-STARRS and the Dark Energy Survey. By comparing higher-$z$ HST data with 42 SN Ia at $z<0.1$ observed in the NIR by the Carnegie Supernova Project, we construct a Hubble diagram from NIR observations (with only time of maximum light and some selection cuts from optical data) to pursue a unique avenue to constrain the dark energy equation of state parameter, $w$. We analyze the dependence of the full set of Hubble residuals on the SN Ia host galaxy mass and find Hubble residual steps of size $\sim$0.06-0.1~mag with 1.5- to 2.5-$蟽$ significance depending on the method and step location. Combining our NIR sample with CMB constraints, we find $1+w=-0.17\pm0.12$ (stat$+$syst). The largest systematic errors are the redshift-dependent SN selection biases and the properties of the NIR mass step. We also use these data to measure $H_0=75.9\pm 2.2$ km s$^{-1}$ Mpc$^{-1}$ from stars with geometric distance calibration in the hosts of 8 SNe Ia observed in the NIR versus $H_0=71.2\pm3.8$ km s$^{-1}$ Mpc$^{-1}$ using an inverse distance ladder approach tied to Planck. Using optical data we find $1+w=-0.10\pm0.09$ and with optical and NIR data combined, we find $1+w=-0.06\pm0.07$; these shifts of up to 0.11 in $w$ could point to inconsistency in optical versus NIR SN models. There will be many opportunities to improve this NIR measurement and better understand systematic uncertainties through larger low-$z$ samples, new light-curve models, calibration improvements, and by building high-$z$ samples from the Roman Space Telescope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.07801v2-abstract-full').style.display = 'none'; document.getElementById('2201.07801v2-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Updated cosmology constraints and text to match published version, and with data release at https://github.com/djones1040/RAISIN_DataRelease</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 933, 172J, 2022 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.04597">arXiv:2112.04597</a> <span> [<a href="https://arxiv.org/pdf/2112.04597">pdf</a>, <a href="https://arxiv.org/format/2112.04597">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac41d3">10.3847/1538-4365/ac41d3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> H-band light curves of Milky Way Cepheids via Difference Imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Konchady%2C+T">Tarini Konchady</a>, <a href="/search/astro-ph?searchtype=author&query=Oelkers%2C+R+J">Ryan J. Oelkers</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+D+O">David O. Jones</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=Peterson%2C+E+R">Erik R. Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.04597v2-abstract-short" style="display: inline;"> We present H-band light curves of Milky Way Classical Cepheids observed as part of the DEHVILS survey with the Wide-Field Infrared Camera on the United Kingdom InfraRed Telescope. Due to the crowded nature of these fields caused by defocusing the Camera, we performed difference-imaging photometry by modifying a pipeline originally developed to analyze images from the Transiting Exoplanet Survey Sa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.04597v2-abstract-full').style.display = 'inline'; document.getElementById('2112.04597v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.04597v2-abstract-full" style="display: none;"> We present H-band light curves of Milky Way Classical Cepheids observed as part of the DEHVILS survey with the Wide-Field Infrared Camera on the United Kingdom InfraRed Telescope. Due to the crowded nature of these fields caused by defocusing the Camera, we performed difference-imaging photometry by modifying a pipeline originally developed to analyze images from the Transiting Exoplanet Survey Satellite. We achieved a photometric precision in line with expectations from photon statistics, reaching 0.01 mag for 8 <= H <= 11 mag. We used the resulting Cepheid light curves to derive corrections to "mean light" for random-phase Hubble Space Telescope observations in F160W. We find good agreement with previous phase corrections based on VI light curves from the literature, with a mean difference of -1 +/- 6 millimag. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.04597v2-abstract-full').style.display = 'none'; document.getElementById('2112.04597v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal Supplement Series. 14 pages, 6 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/2112.04510">arXiv:2112.04510</a> <span> [<a href="https://arxiv.org/pdf/2112.04510">pdf</a>, <a href="https://arxiv.org/format/2112.04510">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/10.3847/2041-8213/ac5c5b">10.3847/2041-8213/ac5c5b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km/s/Mpc Uncertainty from the Hubble Space Telescope and the SH0ES Team </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=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=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=Casertano%2C+S">Stefano Casertano</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=Murakami%2C+Y">Yukei Murakami</a>, <a href="/search/astro-ph?searchtype=author&query=Breuval%2C+L">Louise Breuval</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+T+G">Thomas G. Brink</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=Hoffmann%2C+S">Samantha Hoffmann</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=Kenworthy%2C+W+D">W. D'arcy Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G">Gagandeep Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Mackenty%2C+J">John Mackenty</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=Zheng%2C+W">Weikang Zheng</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.04510v3-abstract-short" style="display: inline;"> We report observations from HST of Cepheids in the hosts of 42 SNe Ia used to calibrate the Hubble constant (H0). These include all suitable SNe Ia in the last 40 years at z<0.01, measured with >1000 orbits, more than doubling the sample whose size limits the precision of H0. The Cepheids are calibrated geometrically from Gaia EDR3 parallaxes, masers in N4258 (here tripling that Cepheid sample), a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.04510v3-abstract-full').style.display = 'inline'; document.getElementById('2112.04510v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.04510v3-abstract-full" style="display: none;"> We report observations from HST of Cepheids in the hosts of 42 SNe Ia used to calibrate the Hubble constant (H0). These include all suitable SNe Ia in the last 40 years at z<0.01, measured with >1000 orbits, more than doubling the sample whose size limits the precision of H0. The Cepheids are calibrated geometrically from Gaia EDR3 parallaxes, masers in N4258 (here tripling that Cepheid sample), and DEBs in the LMC. The Cepheids were measured with the same WFC3 instrument and filters (F555W, F814W, F160W) to negate zeropoint errors. We present multiple verifications of Cepheid photometry and tests of background determinations that show measurements are accurate in the presence of crowding. The SNe calibrate the mag-z relation from the new Pantheon+ compilation, accounting here for covariance between all SN data, with host properties and SN surveys matched to negate differences. We decrease the uncertainty in H0 to 1 km/s/Mpc with systematics. We present a comprehensive set of ~70 analysis variants to explore the sensitivity of H0 to selections of anchors, SN surveys, z range, variations in the analysis of dust, metallicity, form of the P-L relation, SN color, flows, sample bifurcations, and simultaneous measurement of H(z). Our baseline result from the Cepheid-SN sample is H0=73.04+-1.04 km/s/Mpc, which includes systematics and lies near the median of all analysis variants. We demonstrate consistency with measures from HST of the TRGB between SN hosts and NGC 4258 with Cepheids and together these yield 72.53+-0.99. Including high-z SN Ia we find H0=73.30+-1.04 with q0=-0.51+-0.024. We find a 5-sigma difference with H0 predicted by Planck+LCDM, with no indication this arises from measurement errors or analysis variations considered to date. The source of this now long-standing discrepancy between direct and cosmological routes to determining the Hubble constant remains unknown. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.04510v3-abstract-full').style.display = 'none'; document.getElementById('2112.04510v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">67 pages, 31 figures, replaced to match ApJ accepted version (March 2022), Table 6 distances included here, long form of photometry tables, fitting code, compact form of data, available from Github page, https://pantheonplussh0es.github.io</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.03863">arXiv:2112.03863</a> <span> [<a href="https://arxiv.org/pdf/2112.03863">pdf</a>, <a href="https://arxiv.org/format/2112.03863">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/ac8b7a">10.3847/1538-4357/ac8b7a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pantheon+ Analysis: The Full Dataset and Light-Curve Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Carr%2C+A">Anthony Carr</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=Davis%2C+T+M">Tamara M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Dwomoh%2C+A">Arianna Dwomoh</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=Ali%2C+N">Noor Ali</a>, <a href="/search/astro-ph?searchtype=author&query=Charvu%2C+P">Pranav Charvu</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">Rebecca Chen</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=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=Wood%2C+C">Charlotte Wood</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+P+J">Peter J. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Chambers%2C+K">Ken Chambers</a>, <a href="/search/astro-ph?searchtype=author&query=Coulter%2C+D+A">David A. Coulter</a>, <a href="/search/astro-ph?searchtype=author&query=Dettman%2C+K+G">Kyle G. Dettman</a>, <a href="/search/astro-ph?searchtype=author&query=Dimitriadis%2C+G">Georgios Dimitriadis</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=Foley%2C+R+J">Ryan J. Foley</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=Kilpatrick%2C+C+D">Charles D. Kilpatrick</a>, <a href="/search/astro-ph?searchtype=author&query=Kirshner%2C+R+P">Robert P. Kirshner</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Y">Yen-Chen Pan</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.03863v2-abstract-short" style="display: inline;"> Here we present 1701 light curves of 1550 spectroscopically confirmed Type Ia supernovae (SNe Ia) that will be used to infer cosmological parameters as part of the Pantheon+ SN analysis and the SH0ES (Supernovae and H0 for the Equation of State of dark energy) distance-ladder analysis. This effort is one part of a series of works that perform an extensive review of redshifts, peculiar velocities,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.03863v2-abstract-full').style.display = 'inline'; document.getElementById('2112.03863v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.03863v2-abstract-full" style="display: none;"> Here we present 1701 light curves of 1550 spectroscopically confirmed Type Ia supernovae (SNe Ia) that will be used to infer cosmological parameters as part of the Pantheon+ SN analysis and the SH0ES (Supernovae and H0 for the Equation of State of dark energy) distance-ladder analysis. This effort is one part of a series of works that perform an extensive review of redshifts, peculiar velocities, photometric calibration, and intrinsic-scatter models of SNe Ia. The total number of light curves, which are compiled across 18 different surveys, is a significant increase from the first Pantheon analysis (1048 SNe), particularly at low redshift ($z$). Furthermore, unlike in the Pantheon analysis, we include light curves for SNe with $z<0.01$ such that SN systematic covariance can be included in a joint measurement of the Hubble constant (H$_0$) and the dark energy equation-of-state parameter ($w$). We use the large sample to compare properties of 151 SNe Ia observed by multiple surveys and 12 pairs/triplets of "SN siblings" - SNe found in the same host galaxy. Distance measurements, application of bias corrections, and inference of cosmological parameters are discussed in the companion paper by Brout et al. (2022b), and the determination of H$_0$ is discussed by Riess et al. (2022). These analyses will measure w with $\sim3\%$ precision and H$_0$ with 1 km/s/Mpc precision. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.03863v2-abstract-full').style.display = 'none'; document.getElementById('2112.03863v2-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 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJL. Comments welcome. Papers and data release here: https://github.com/PantheonPlusSH0ES/PantheonPlusSH0ES.github.io</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.03081">arXiv:2111.03081</a> <span> [<a href="https://arxiv.org/pdf/2111.03081">pdf</a>, <a href="https://arxiv.org/format/2111.03081">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"> A Reference Survey for Supernova Cosmology with the Nancy Grace Roman Space Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rose%2C+B+M">B. M. Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Hounsell%2C+R">R. Hounsell</a>, <a href="/search/astro-ph?searchtype=author&query=Macias%2C+P">P. Macias</a>, <a href="/search/astro-ph?searchtype=author&query=Rubin%2C+D">D. Rubin</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Aldering%2C+G">G. Aldering</a>, <a href="/search/astro-ph?searchtype=author&query=Bohlin%2C+R">R. Bohlin</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+M">M. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Deustua%2C+S+E">S. E. Deustua</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=Fruchter%2C+A">A. Fruchter</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</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=Jones%2C+D+O">D. O. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+B+A">B. A. Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Kelly%2C+P+L">P. L. Kelly</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</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=Mandel%2C+K+S">K. S. Mandel</a>, <a href="/search/astro-ph?searchtype=author&query=Perlmutter%2C+S">S. Perlmutter</a>, <a href="/search/astro-ph?searchtype=author&query=Pierel%2C+J">J. Pierel</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">H. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Rabinowitz%2C+D">D. Rabinowitz</a>, <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">A. Rest</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.03081v1-abstract-short" style="display: inline;"> This note presents an initial survey design for the Nancy Grace Roman High-latitude Time Domain Survey. This is not meant to be a final or exhaustive list of all the survey strategy choices, but instead presents a viable path towards achieving the desired precision and accuracy of dark energy measurements using Type Ia supernovae (SNe Ia). We describe a survey strategy that use six filters (RZYJH… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.03081v1-abstract-full').style.display = 'inline'; document.getElementById('2111.03081v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.03081v1-abstract-full" style="display: none;"> This note presents an initial survey design for the Nancy Grace Roman High-latitude Time Domain Survey. This is not meant to be a final or exhaustive list of all the survey strategy choices, but instead presents a viable path towards achieving the desired precision and accuracy of dark energy measurements using Type Ia supernovae (SNe Ia). We describe a survey strategy that use six filters (RZYJH and F) and the prism on the Roman Wide Field Instrument. This survey has two tiers, one "wide" which targets SNe Ia at redshifts up to 1 and one "deep" targeting redshifts up to 1.7; for each, four filters are used (with Y and J used in both tiers). We propose one field each in the north and south continuous viewing zones, and expect to obtain high-quality distances of $\sim$12,000 SNe Ia with $\sim$5,000 at z > 1. We propose a wide-tier area of $\sim$19 deg$^2$ and a deep tier of $\sim$5 deg$^2$. Exposure times range from 100 s to 900 s for imaging and 900 s to 3600 s for the prism. These exposure times would reach $\sim$25.5 mag and $\sim$26.5 mag for the wide and deep tiers respectively, with deep co-add stacks reaching $\sim$28 mag and $\sim$29 mag. The total survey spans two years, with a total allocation time of six months, and a cadence of $\sim$5 days. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.03081v1-abstract-full').style.display = 'none'; document.getElementById('2111.03081v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A report to NASA from the Roman Supernova Science Investigation Teams</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.03487">arXiv:2110.03487</a> <span> [<a href="https://arxiv.org/pdf/2110.03487">pdf</a>, <a href="https://arxiv.org/format/2110.03487">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/ac4698">10.3847/1538-4357/ac4698 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pantheon+ Analysis: Evaluating Peculiar Velocity Corrections in Cosmological Analyses with Nearby Type Ia Supernovae </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=Kenworthy%2C+W+D">W. D'Arcy Kenworthy</a>, <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=Brout%2C+D">Dillon Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+A">Anthony Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Courtois%2C+H">Helene Courtois</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T">Tamara Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Dwomoh%2C+A">Arianna Dwomoh</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=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=Said%2C+K">Khaled Said</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.03487v2-abstract-short" style="display: inline;"> Separating the components of redshift due to expansion and peculiar motion in the nearby universe ($z<0.1$) is critical for using Type Ia Supernovae (SNe Ia) to measure the Hubble constant ($H_0$) and the equation-of-state parameter of dark energy ($w$). Here, we study the two dominant 'motions' contributing to nearby peculiar velocities: large-scale, coherent-flow (CF) motions and small-scale mot… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.03487v2-abstract-full').style.display = 'inline'; document.getElementById('2110.03487v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.03487v2-abstract-full" style="display: none;"> Separating the components of redshift due to expansion and peculiar motion in the nearby universe ($z<0.1$) is critical for using Type Ia Supernovae (SNe Ia) to measure the Hubble constant ($H_0$) and the equation-of-state parameter of dark energy ($w$). Here, we study the two dominant 'motions' contributing to nearby peculiar velocities: large-scale, coherent-flow (CF) motions and small-scale motions due to gravitationally associated galaxies deemed to be in a galaxy group. We use a set of 584 low-$z$ SNe from the Pantheon+ sample, and evaluate the efficacy of corrections to these motions by measuring the improvement of SN distance residuals. We study multiple methods for modeling the large and small-scale motions and show that, while group assignments and CF corrections individually contribute to small improvements in Hubble residual scatter, the greatest improvement comes from the combination of the two (relative standard deviation of the Hubble residuals, Rel. SD, improves from 0.167 to 0.157 mag). We find the optimal flow corrections derived from various local density maps significantly reduce Hubble residuals while raising $H_0$ by $\sim0.4$ km s$^{-1}$ Mpc$^{-1}$ as compared to using CMB redshifts, disfavoring the hypothesis that unrecognized local structure could resolve the Hubble tension. We estimate that the systematic uncertainties in cosmological parameters after optimally correcting redshifts are 0.06-0.11 km s$^{-1}$ Mpc$^{-1}$ in $H_0$ and 0.02-0.03 in $w$ which are smaller than the statistical uncertainties for these measurements: 1.5 km s$^{-1}$ Mpc$^{-1}$ for $H_0$ and 0.04 for $w$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.03487v2-abstract-full').style.display = 'none'; document.getElementById('2110.03487v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 9 figures. 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/2110.03486">arXiv:2110.03486</a> <span> [<a href="https://arxiv.org/pdf/2110.03486">pdf</a>, <a href="https://arxiv.org/format/2110.03486">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 Pantheon+ Analysis: Dependence of Cosmological Constraints on Photometric-Zeropoint Uncertainties of Supernova Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brownsberger%2C+S">Sasha Brownsberger</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">Dillon Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Stubbs%2C+C+W">Christopher W. Stubbs</a>, <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.03486v1-abstract-short" style="display: inline;"> Type Ia supernovae (SNe Ia) measurements of the Hubble constant, H$_0$, the cosmological mass density, $惟_M$, and the dark energy equation-of-state parameter, $w$, rely on numerous SNe surveys using distinct photometric systems across three decades of observation. Here, we determine the sensitivities of the upcoming SH0ES+Pantheon+ constraints on H$_0$, $惟_M$, and $w$ to unknown systematics in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.03486v1-abstract-full').style.display = 'inline'; document.getElementById('2110.03486v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.03486v1-abstract-full" style="display: none;"> Type Ia supernovae (SNe Ia) measurements of the Hubble constant, H$_0$, the cosmological mass density, $惟_M$, and the dark energy equation-of-state parameter, $w$, rely on numerous SNe surveys using distinct photometric systems across three decades of observation. Here, we determine the sensitivities of the upcoming SH0ES+Pantheon+ constraints on H$_0$, $惟_M$, and $w$ to unknown systematics in the relative photometric zeropoint calibration between the 17 surveys that comprise the Pantheon+ supernovae data set. Varying the zeropoints of these surveys simultaneously with the cosmological parameters, we determine that the SH0ES+Pantheon+ measurement of H$_0$ is robust against inter-survey photometric miscalibration, but that the measurements of $惟_M$ and $w$ are not. Specifically, we find that miscalibrated inter-survey systematics could represent a source of uncertainty in the measured value of H$_0$ that is no larger than $0.2$ km s$^{-1}$ Mpc$^{-1}$. This modest increase in H$_0$ uncertainty could not account for the $7$ km s$^{-1}$ Mpc$^{-1}$ "Hubble Tension" between the SH0ES measurement of H$_0$ and the Planck $螞$CDM-based inference of H$_0$. However, we find that the SH0ES+Pantheon+ best-fit values of $惟_M$ and $w$ respectively slip, to first order, by $0.04$ and $-0.17$ per $25$ mmag of inter-survey calibration uncertainty, underscoring the vital role that cross-calibration plays in accurately measuring these parameters. Because the Pantheon+ compendium contains many surveys that share low-$z$ Hubble Flow and Cepheid-paired SNe, the SH0ES+Pantheon+ joint constraint of H$_0$ is robust against inter-survey photometric calibration errors, and such errors do not represent an impediment to jointly using SH0ES+Pantheon+ to measure H$_0$ to 1% accuracy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.03486v1-abstract-full').style.display = 'none'; document.getElementById('2110.03486v1-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/2108.00007">arXiv:2108.00007</a> <span> [<a href="https://arxiv.org/pdf/2108.00007">pdf</a>, <a href="https://arxiv.org/format/2108.00007">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/ac68df">10.3847/1538-4357/ac68df <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Comparing Tip of the Red Giant Branch Distance Scales: An Independent Reduction of the Carnegie-Chicago Hubble Program and the Value of the Hubble Constant </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=Tully%2C+R+B">R. Brent Tully</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzi%2C+L">Luca Rizzi</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> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.00007v2-abstract-short" style="display: inline;"> The tip of the red giant branch has been used to measure distances to 500 nearby galaxies with the Hubble Space Telescope (HST) which are available in the Color-Magnitude Diagrams and Tip of the Red Giant Branch (CMDs/TRGB) catalog on the Extragalactic Distance Database (EDD). Our established methods are employed to perform an independent reduction of the targets presented by the Carnegie-Chicago… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.00007v2-abstract-full').style.display = 'inline'; document.getElementById('2108.00007v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.00007v2-abstract-full" style="display: none;"> The tip of the red giant branch has been used to measure distances to 500 nearby galaxies with the Hubble Space Telescope (HST) which are available in the Color-Magnitude Diagrams and Tip of the Red Giant Branch (CMDs/TRGB) catalog on the Extragalactic Distance Database (EDD). Our established methods are employed to perform an independent reduction of the targets presented by the Carnegie-Chicago Hubble Program (CCHP) in the series of papers culminating in Freedman (2021). Our distinct methodology involves modeling the observed luminosity function of red giant branch and asymptotic giant branch stars, which differs from the edge-detection algorithms employed by the CCHP. We find excellent agreement between distances for 11 hosts with new imaging, all at D < 20 Mpc. However, we are unable to measure the TRGB for 4 of the 5 hosts that use archival data designed to measure distances with Cepheids, all at D > 23 Mpc. With two new HST observations taken in the halo of the megamaser host NGC 4258, the first with the same ACS F606W and F814W filters and the post-servicing electronics used for SN Ia hosts, we then calibrate our TRGB distance scale to the geometric megamaser distance. Using our TRGB distances, we find a value of the Hubble Constant of $H_{0}$ = 71.5 $\pm$ 1.8 km/s/Mpc when using either the Pantheon or Carnegie Supernova Project (CSP) samples of supernovae. In the future, the James Webb Space Telescope will extend measurements of the TRGB to additional hosts of SN Ia and surface brightness fluctuation measurements for separate paths to $H_{0}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.00007v2-abstract-full').style.display = 'none'; document.getElementById('2108.00007v2-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" 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