Examinando por Autor "Papovich, C."

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Acceso Abierto
Implications of Increased Central Mass Surface Densities for the Quenching of Low-mass Galaxies
(IOP Science Publishing, 2021-06-08) Guo, Y.; Carleton, T.; Bell, E. F.; Chen, Z.; Dekel, A.; Faber, S. M.; Giavalisco, M.; Kocevski, D. D.; Koekemoer, A. M.; Koo, D. C.; Kurczynski, P.; Lee, S. K.; Liu, F. S.; Papovich, C.; Pérez González, G.; National Science Foundation (NSF); National Aeronautics and Space Administration (NASA); National Research Foundation of Korea (NRF); Guo, Y. [0000-0003-2775-2002]; Carleton, T. [0000-0001-6650-2853]; Bell, E. F. [0000-0002-5564-9873]; Chen, Z. [0000-0002-2326-0476]; Dekel, A. [0000-0003-4174-0374]; Fabel, S. M. [0000-0003-4996-214X]; Giavalisco, M. [0000-0002-7831-8751]; Kocevski, D. D. [0000-0002-8360-3880]; Koekemoer, A. M. [0000-0002-6610-2048]; Koo, D. C. [0000-0003-3385-6799]; Kurczynski, P. [0000-0002-8816-5146]; Lee, S. K. [0000-0001-5342-8906]; Liu, F. S. [0000-0002-1064-1544]; Papovich, C. [0000-0001-7503-8482]; Pérez González, P. G. [0000-0003-4528-5639]
We use the Cosmic Assembly Deep Near-infrared Extragalactic Legacy Survey data to study the relationship between quenching and the stellar mass surface density within the central radius of 1 kpc (Σ1) of low-mass galaxies (stellar mass M* ≲ 109.5 M⊙) at 0.5 ≤ z < 1.5. Our sample is mass complete down to ∼109 M⊙ at 0.5 ≤ z < 1.0. We compare the mean Σ1 of star-forming galaxies (SFGs) and quenched galaxies (QGs) at the same redshift and M*. We find that low-mass QGs have a higher Σ1 than low-mass SFGs, similar to galaxies above 1010 M⊙. The difference of Σ1 between QGs and SFGs increases slightly with M* at M* ≲ 1010 M⊙ and decreases with M* at M* ≳ 1010 M⊙. The turnover mass is consistent with the mass where quenching mechanisms transition from internal to environmental quenching. At 0.5 ≤ z < 1.0, we find that Σ1 of galaxies increases by about 0.25 dex in the green valley (i.e., the transition region from star forming to fully quenched), regardless of their M*. Using the observed specific star formation rate gradient in the literature as a constraint, we estimate that the quenching timescale (i.e., time spent in the transition) of low-mass galaxies is a few (∼4) Gyr at 0.5 ≤ z < 1.0. The mechanisms responsible for quenching need to gradually quench star formation in an outside-in way, i.e., preferentially ceasing star formation in outskirts of galaxies while maintaining their central star formation to increase Σ1. An interesting and intriguing result is the similarity of the growth of Σ1 in the green valley between low-mass and massive galaxies, which suggests that the role of internal processes in quenching low-mass galaxies is a question worthy of further investigation.
Acceso Abierto
JWST/MIRI Simulated Imaging: Insights into Obscured Star Formation and AGNs for Distant Galaxies in Deep Surveys
(IOP Science Publishing, 2021-02-19) Yang, C.; Papovich, C.; Bagley, M. B.; Buat, V.; Burgarella, D.; Dickinson, M.; Elbaz, D.; Finkelstein, S.; Fontana, A.; Grogin, N. A.; Jung, I.; Kartaltepe, J. S.; Kirkpatrick, A.; Koekemoer, A. M.; Pérez González, P. G.; Pirzkal, N.; Yung, L. Y. A.; Yang, C. [0000-0001-8835-7722]; Papovich, C. [0000-0001-7503-8482]; Bagley, M. B. [0000-0002-9921-9218]; Buat, V. [0000-0003-3441-903X]; Burgarella, D. [0000-0002-4193-2539]; Dickinson, M. [0000-0001-5414-5131]; Finkelstein, S. L. [0000-0001-8519-1130]; Fontana, A. [0000-0003-3820-2823]; Grogin, N. A. [0000-0001-9440-8872]; Jung, I. [0000-0003-1187-4240]; Kartaltepe, J. S. [0000-0001-9187-3605]; Kirkpatrick, A. [0000-0002-1306-1545]; Koekemoer, A. M. [0000-0002-6610-2048]; Pérez González, P. G. [0000-0003-4528-5639]; Yung, L. Y. A. [0000-0003-3466-035X]
The James Webb Space Telescope MIRI instrument will revolutionize extragalactic astronomy with unprecedented sensitivity and angular resolution in mid-IR. Here we assess the potential of MIRI photometry to constrain galaxy properties in the Cosmic Evolution Early Release Science (CEERS) survey. We derive estimated MIRI fluxes from the spectral energy distributions (SEDs) of real sources that fall in a planned MIRI pointing. We also obtain MIRI fluxes for hypothetical active galactic nucleus (AGN)–galaxy mixed models varying the AGN fractional contribution to the total IR luminosity (fracAGN). Based on these model fluxes, we simulate CEERS imaging (3.6 hr exposure) in six bands from F770W to F2100W using mirisim and reduce these data using jwst pipeline. We perform point-spread-function-matched photometry with tphot and fit the source SEDs with x-cigale, simultaneously modeling photometric redshift and other physical properties. Adding the MIRI data, the accuracy of both redshift and fracAGN is generally improved by factors of ≳2 for all sources at z ≲ 3. Notably, for pure-galaxy inputs (fracAGN = 0), the accuracy of fracAGN is improved by ∼100 times thanks to MIRI. The simulated CEERS MIRI data are slightly more sensitive to AGN detections than the deepest X-ray survey, based on the empirical LX–L6 μm relation. Like X-ray observations, MIRI can also be used to constrain the AGN accretion power (accuracy ≈0.3 dex). Our work demonstrates that MIRI will be able to place strong constraints on the mid-IR luminosities from star formation and AGNs and thereby facilitate studies of the galaxy/AGN coevolution.