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59 results on '"Estrada-Carpenter, Vicente"'

51. Evidence for Early Formation of the Most Compact Quiescent Galaxies at High Redshift Using Deep Hubble Grism Data

Author

Estrada-Carpenter, Vicente

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The origin of the correlations between mass, morphology, and formation history in galaxies is difficult to define, primarily due to uncertainties in galaxy star-formation histories, which are better constrained for higher redshift galaxies. Here we use a forward modeling technique on deep HST grism data (a method which can be applied to grism data from the Nancy Grace Roman Space Telescope) from the CLEAR (CANDELS Lyα Emission at Reionization) survey. We derive constraints on the formation and quenching timescales of quiescent galaxies at 0.7 < z < 2.5 using “non-parametric” star-formation histories. The galaxy formation redshifts, z50 (defined as the point where they formed 50% of their stellar mass) range from z50 ~ 2 (shortly prior to the observed epoch) up to z50 ~ 5-8. We find that early formation redshifts are correlated with high stellar-mass surface densities, log(Σ1) > 10.25, where Σ1 is the stellar mass within 1 proper kpc. Quiescent galaxies with the highest stellar-mass surface density, log(Σ1) > 10.25, show a minimum formation redshift: all such objects in our sample have z50 > 2.9. Quiescent galaxies with lower surface density show a range of formation epochs (z50 ~ 1.5 - 8), implying these galaxies experienced a range of formation and assembly histories. We argue that the surface density threshold log(Σ1) > 10.25 uniquely identifies galaxies that formed in the first few Gyr after the big bang, and discuss the implications this has for galaxy formation models.

Published
2021
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52. CLEAR:The Gas-phase Metallicity Gradients of Star-forming Galaxies at 0.6 < z < 2.6

Author

Simons, Raymond C., Papovich, Casey, Momcheva, Ivelina, Trump, Jonathan R., Brammer, Gabriel, Estrada-Carpenter, Vicente, Backhaus, Bren E., Cleri, Nikko J., Finkelstein, Steven L., Giavalisco, Mauro, Ji, Zhiyuan, Jung, Intae, Matharu, Jasleen, Weiner, Benjamin, Simons, Raymond C., Papovich, Casey, Momcheva, Ivelina, Trump, Jonathan R., Brammer, Gabriel, Estrada-Carpenter, Vicente, Backhaus, Bren E., Cleri, Nikko J., Finkelstein, Steven L., Giavalisco, Mauro, Ji, Zhiyuan, Jung, Intae, Matharu, Jasleen, and Weiner, Benjamin

Abstract

We report on the gas-phase metallicity gradients of a sample of 238 star-forming galaxies at 0.6 < z < 2.6, measured through deep near-infrared Hubble Space Telescope slitless spectroscopy. The observations include 12 orbit depth Hubble/WFC3 G102 grism spectra taken as a part of the CANDELS Ly alpha Emission at Reionization (CLEAR) survey, and archival WFC3 G102+G141 grism spectra overlapping the CLEAR footprint. The majority of galaxies in this sample are consistent with having a zero or slightly positive metallicity gradient (dZ/dR >= 0, i.e., increasing with radius) across the full mass range probed (8.5 < log M (*)/M (circle dot) < 10.5). We measure the intrinsic population scatter of the metallicity gradients, and show that it increases with decreasing stellar mass-consistent with previous reports in the literature, but confirmed here with a much larger sample. To understand the physical mechanisms governing this scatter, we search for correlations between the observed gradient and various stellar population properties at fixed mass. However, we find no evidence for a correlation with the galaxy properties we consider-including star formation rates, sizes, star formation rate surface densities, and star formation rates per gravitational potential energy. We use the observed weakness of these correlations to provide material constraints for predicted intrinsic correlations from theoretical models.

Published
2021

53. CLEAR: Boosted Ly α Transmission of the Intergalactic Medium in UV-bright Galaxies.

Author

Jung, Intae, Papovich, Casey, Finkelstein, Steven L., Simons, Raymond C., Estrada-Carpenter, Vicente, Backhaus, Bren E., Cleri, Nikko J., Finlator, Kristian, Giavalisco, Mauro, Ji, Zhiyuan, Matharu, Jasleen, Momcheva, Ivelina, Straughn, Amber N., and Trump, Jonathan R.

Subjects
GALAXIES, REDSHIFT, GALAXY spectra, SPACE telescopes, GALACTIC redshift, STELLAR luminosity function, SPECTROGRAPHS, INTERSTELLAR medium
Abstract

Reionization is an inhomogeneous process, thought to begin in small ionized bubbles of the intergalactic medium (IGM) around overdense regions of galaxies. Recent Ly α studies during the epoch of reionization show evidence that ionized bubbles formed earlier around brighter galaxies, suggesting higher IGM transmission of Ly α from these galaxies. We investigate this problem using IR slitless spectroscopy from the Hubble Space Telescope (HST) Wide-Field Camera 3 (WFC3) G102 grism observations of 148 galaxies selected via photometric redshifts at 6.0 < z < 8.2. These galaxies have spectra extracted from the CANDELS Ly α Emission at Reionization (CLEAR) survey. We combine the CLEAR data for 275 galaxies with the Keck Deep Imaging Multi-Object Spectrograph and MOSFIRE data set from the Texas Spectroscopic Search for Ly α Emission at the End of Reionization Survey. We constrain the Ly α equivalent width (EW) distribution at 6.0 < z < 8.2, which is described by an exponential form, dN / d EW ∝ exp (âˆ' EW) / W 0 , with the characteristic e -folding scale width (W 0). We confirm a significant drop in the Ly α strength (i.e., W 0) at z > 6. Furthermore, we compare the redshift evolution of W 0 between galaxies at different UV luminosities. UV-bright (M UV < âˆ'21 [i.e., L UV > L *]) galaxies show weaker evolution with a decrease of 0.4 (± 0.2) dex in W 0 at z > 6, while UV-faint (M UV > âˆ'21 [ L UV < L *]) galaxies exhibit a significant drop of 0.7â€"0.8 (±0.2) dex in W 0 from z < 6 to z > 6. If the change in W 0 is proportional to the change in the IGM transmission for Ly α photons, then this is evidence that the transmission is “boosted” around UV-brighter galaxies, suggesting that reionization proceeds faster in regions around such galaxies. [ABSTRACT FROM AUTHOR]

Published
2022
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54. CLEAR: Paschen- β Star Formation Rates and Dust Attenuation of Low-redshift Galaxies.

Author

Cleri, Nikko J., Trump, Jonathan R., Backhaus, Bren E., Momcheva, Ivelina, Papovich, Casey, Simons, Raymond, Weiner, Benjamin, Estrada-Carpenter, Vicente, Finkelstein, Steven L., Giavalisco, Mauro, Ji, Zhiyuan, Jung, Intae, Matharu, Jasleen, Martinez III, Felix, and Sturm, Megan R.

Subjects
STAR formation, GALAXIES, SPECTRAL energy distribution, DUST, STELLAR mass, SPACE telescopes, COSMIC dust
Abstract

We use Paschen- β (Pa β ; 1282 nm) observations from the Hubble Space Telescope G141 grism to study the star formation and dust-attenuation properties of a sample of 29 low-redshift (z < 0.287) galaxies in the CANDELS Ly α Emission at Reionization survey. We first compare the nebular attenuation from Pa β /H α with the stellar attenuation inferred from the spectral energy distribution, finding that the galaxies in our sample are consistent with an average ratio of the continuum attenuation to the nebular gas of 0.44, but with a large amount of excess scatter beyond the observational uncertainties. Much of this scatter is linked to a large variation between the nebular dust attenuation as measured by (space-based) Pa β to (ground-based) H α to that from (ground-based) H α /H β. This implies there are important differences between attenuation measured from grism-based/wide-aperture Pa β fluxes and the ground-based/slit-measured Balmer decrement. We next compare star formation rates (SFRs) from Pa β to those from dust-corrected UV. We perform a survival analysis to infer a census of Pa β emission implied by both detections and nondetections. We find evidence that galaxies with lower stellar mass have more scatter in their ratio of Pa β to attenuation-corrected UV SFRs. When considering our Pa β detection limits, this observation supports the idea that lower-mass galaxies experience “burstier” star formation histories. Together, these results show that Pa β is a valuable tracer of a galaxy’s SFR, probing different timescales of star formation and potentially revealing star formation that is otherwise missed by UV and optical tracers. [ABSTRACT FROM AUTHOR]

Published
2022
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55. CLEAR. II. Evidence for Early Formation of the Most Compact Quiescent Galaxies at High Redshift

Author

Estrada-Carpenter, Vicente, primary, Papovich, Casey, additional, Momcheva, Ivelina, additional, Brammer, Gabriel, additional, Simons, Raymond, additional, Bridge, Joanna, additional, Cleri, Nikko J., additional, Ferguson, Henry, additional, Finkelstein, Steven L., additional, Giavalisco, Mauro, additional, Jung, Intae, additional, Matharu, Jasleen, additional, Trump, Jonathan R., additional, and Weiner, Benjamin, additional

Published
2020
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56. CLEAR. I. Ages and Metallicities of Quiescent Galaxies at 1.0 < z < 1.8 Derived from Deep Hubble Space Telescope Grism Data

Author

Estrada-Carpenter, Vicente, primary, Papovich, Casey, additional, Momcheva, Ivelina, additional, Brammer, Gabriel, additional, Long, James, additional, Quadri, Ryan F., additional, Bridge, Joanna, additional, Dickinson, Mark, additional, Ferguson, Henry, additional, Finkelstein, Steven, additional, Giavalisco, Mauro, additional, Gosmeyer, Catherine M., additional, Lotz, Jennifer, additional, Salmon, Brett, additional, Skelton, Rosalind E., additional, Trump, Jonathan R., additional, and Weiner, Benjamin, additional

Published
2019
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57. SPITZER SPACE TELESCOPEMEASUREMENTS OF DUST REVERBERATION LAGS IN THE SEYFERT 1 GALAXY NGC 6418

Author

Vazquez, Billy, primary, Galianni, Pasquale, additional, Richmond, Michael, additional, Robinson, Andrew, additional, Axon, David J., additional, Horne, Keith, additional, Almeyda, Triana, additional, Fausnaugh, Michael, additional, Peterson, Bradley M., additional, Bottorff, Mark, additional, Gallimore, Jack, additional, Eltizur, Moshe, additional, Netzer, Hagai, additional, Storchi-Bergmann, Thaisa, additional, Marconi, Alessandro, additional, Capetti, Alessandro, additional, Batcheldor, Dan, additional, Buchanan, Catherine, additional, Stirpe, Giovanna, additional, Kishimoto, Makoto, additional, Packham, Christopher, additional, Perez, Enrique, additional, Tadhunter, Clive, additional, Upton, John, additional, and Estrada-Carpenter, Vicente, additional

Published
2015
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58. A Long Time Ago in a Galaxy Far, Far Away: A Candidate z similar to 12 Galaxy in Early JWST CEERS Imaging

Author

Finkelstein, Steven L., Bagley, Micaela B., Haro, Pablo Arrabal, Dickinson, Mark, Ferguson, Henry C., Kartaltepe, Jeyhan S., Papovich, Casey, Burgarella, Denis, Kocevski, Dale D., Huertas-Company, Marc, Iyer, Kartheik G., Koekemoer, Anton M., Larson, Rebecca L., Perez-Gonzalez, Pablo G., Rose, Caitlin, Tacchella, Sandro, Wilkins, Stephen M., Chworowsky, Katherine, Medrano, Aubrey, Morales, Alexa M., Somerville, Rachel S., Yung, L. Y. Aaron, Fontana, Adriano, Giavalisco, Mauro, Grazian, Andrea, Grogin, Norman A., Kewley, Lisa J., Kirkpatrick, Allison, Kurczynski, Peter, Lotz, Jennifer M., Pentericci, Laura, Pirzkal, Nor, Ravindranath, Swara, Ryan, Russell E., Jr., Trump, Jonathan R., Yang, Guang, Almaini, Omar, Amorin, Ricardo O., Annunziatella, Marianna, Backhaus, Bren E., Barro, Guillermo, Behroozi, Peter, Bell, Eric F., Bhatawdekar, Rachana, Bisigello, Laura, Bromm, Volker, Buat, Veronique, Buitrago, Fernando, Calabro, Antonello, Casey, Caitlin M., Castellano, Marco, Ortiz, Oscar A. Chavez, Ciesla, Laure, Cleri, Nikko J., Cohen, Seth H., Cole, Justin W., Cooke, Kevin C., Cooper, M. C., Cooray, Asantha R., Costantin, Luca, Cox, Isabella G., Croton, Darren, Daddi, Emanuele, Dave, Romeel, de la Vega, Alexander, Dekel, Avishai, Elbaz, David, Estrada-Carpenter, Vicente, Faber, Sandra M., Fernandez, Vital, Finkelstein, Keely D., Freundlich, Jonathan, Fujimoto, Seiji, Garcia-Argumanez, Angela, Gardner, Jonathan P., Gawiser, Eric, Gomez-Guijarro, Carlos, Guo, Yuchen, Hamblin, Kurt, Hamilton, Timothy S., Hathi, Nimish P., Holwerda, Benne W., Hirschmann, Michaela, Hutchison, Taylor A., Jaskot, Anne E., Jha, Saurabh W., Jogee, Shardha, Juneau, Stephanie, Jung, Intae, Kassin, Susan A., Le Bail, Aurelien, Leung, Gene C. K., Lucas, Ray A., Magnelli, Benjamin, Mantha, Kameswara Bharadwaj, Matharu, Jasleen, McGrath, Elizabeth J., McIntosh, Daniel H., Merlin, Emiliano, Mobasher, Bahram, Newman, Jeffrey A., Nicholls, David C., Pandya, Viraj, Rafelski, Marc, Ronayne, Kaila, Santini, Paola, Seille, Lise-Marie, Shah, Ekta A., Shen, Lu, Simons, Raymond C., Snyder, Gregory F., Stanway, Elizabeth R., Straughn, Amber N., Teplitz, Harry, I, Vanderhoof, Brittany N., Vega-Ferrero, Jesus, Wang, Weichen, Weiner, Benjamin J., Willmer, Christopher N. A., Wuyts, Stijn, and Zavala, Jorge A.

Subjects
epoch simulations flares, semianalytic forecasts, space-telescope, 1st galaxies, star-formation histories, light-cones, mass, luminosity function, l-dwarf, stellar
Abstract

We report the discovery of a candidate galaxy with a photo -z of z similar to 12 in the first epoch of the James Webb Space Telescope (JWST) Cosmic Evolution Early Release Science Survey. Following conservative selection criteria, we identify a source with a robust zphot = 11.8(+0.3) (-0.2) (1 sigma uncertainty) with m(F200W) = 27.3 and > 7 sigma detections in five filters. The source is not detected at lambda < 1.4 mu m in deep imaging from both Hubble Space Telescope (HST) and JWST and has faint similar to 3 sigma detections in JWST F150W and HST F160W, which signal a Ly alpha break near the red edge of both filters, implying z similar to 12. This object (Maisie's Galaxy) exhibits F115W - F200W > 1.9 mag (2 sigma lower limit) with a blue continuum slope, resulting in 99.6% of the photo-z probability distribution function favoring z > 11. All data-quality images show no artifacts at the candidate's position, and independent analyses consistently find a strong preference for z > 11. Its colors are inconsistent with Galactic stars, and it is resolved (r(h) = 340 +/- 14 pc). Maisie's Galaxy has log M-*/M-?similar to 8.5 and is highly star-forming (log sSFR similar to -8.2 yr(-1)), with a blue rest-UV color (beta similar to -2.5) indicating little dust, though not extremely low metallicity. While the presence of this source is in tension with most predictions, it agrees with empirical extrapolations assuming UV luminosity functions that smoothly decline with increasing redshift. Should follow-up spectroscopy validate this redshift, our universe was already aglow with galaxies less than 400 Myr after the Big Bang.

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