ChinaXiv.org 中国科学院科技论文预发布平台

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2023
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Astrophysical processes
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Your conditions: Pablo G. Pérez-González

1. ChinaXiv:202303.04223
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Life beyond 30: probing the $-20

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Pablo G. Pérez-González Luca Costantin Danial Langeroodi Pierluigi Rinaldi Marianna Annunziatella Olivier Ilbert Luis Colina Hans Ulrik Noorgaard-Nielsen Thomas Greve Göran Ostlin Gillian Wright Almudena Alonso-Herrero Javier Álvarez-Márquez Karina I. Caputi Andreas Eckart Olivier Le Fèvre Álvaro Labiano Macarena García-Marín Jens Hjorth Sarah Kendrew

Abstract： We present the ultraviolet luminosity function and an estimate of the cosmic star formation rate density at $88$ galaxy candidates based on their dropout nature in the $F115W$ and/or $F150W$ filters, a high probability for their photometric redshifts, estimated with three different codes, being at $z>8$, good fits based on $\chi^2$ calculations, and predominant solutions compared to $z<8$ alternatives. We find mild evolution in the luminosity function from $z\sim13$ to $z\sim8$, i.e., only a small increase in the average number density of $\sim$0.2~dex, while the faint-end slope and absolute magnitude of the knee remain approximately constant, with values $\alpha=-2.3\pm0.2$ and $M^*=-20.8\pm0.2$~mag. Comparing our results with the predictions of a wide range of state-of-the-art galaxy evolution models, we find two main results: (1) a slower increase with time in the cosmic star formation rate density compared to a steeper rise predicted by models; (2) nearly a factor of 10 higher star formation activity concentrated in scales around 2~kpc in galaxies with stellar masses $\sim10^8$~M$_\odot$ during the first 350~Myr of the Universe ($z\sim12$), with models matching better the observations $\sim$150~Myr later, by $z\sim9$.

Peer Review Status:Awaiting Review

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2. ChinaXiv:202303.05800
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First Look at z > 1 Bars in the Rest-Frame Near-Infrared with JWST Early CEERS Imaging

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Yuchen Guo Shardha Jogee Steven L. Finkelstein Zilei Chen Eden Wise Micaela B. Bagley Guillermo Barro Stijn Wuyts Dale D. Kocevski Jeyhan S. Kartaltepe Elizabeth J. McGrath Henry C. Ferguson Bahram Mobasher Mauro Giavalisco Ray A. Lucas Jorge A. Zavala Jennifer M. Lotz Norman A. Grogin Marc Huertas-Company Jesús Vega-Ferrero

Abstract： Stellar bars are key drivers of secular evolution in galaxies and can be effectively studied using rest-frame near-infrared (NIR) images, which trace the underlying stellar mass and are less impacted by dust and star formation than rest-frame UV or optical images. We leverage the power of {\it{JWST}} CEERS NIRCam images to present the first quantitative identification and characterization of stellar bars at $z>1$ based on rest-frame NIR F444W images of high resolution (~1.3 kpc at z ~ 1-3). We identify stellar bars in these images using quantitative criteria based on ellipse fits. For this pilot study, we present six examples of robustly identified bars at $z>1$ with spectroscopic redshifts, including the two highest redshift bars at ~2.136 and 2.312 quantitatively identified and characterized to date. The stellar bars at $z$ ~ 1.1-2.3 presented in our study have projected semi-major axes of ~2.9-4.3 kpc and projected ellipticities of ~0.41-0.53 in the rest-frame NIR. The barred host galaxies have stellar masses ~ $ 1 \times 10^{10}$ to $2 \times 10^{11}$ $M_{\odot}$, star formation rates of ~ 21-295 $M_{\odot}$ yr$^{-1}$, and several have potential nearby companions. Our finding of bars at $z$ ~1.1-2.3 demonstrates the early onset of such instabilities and supports simulations where bars form early in massive dynamically cold disks. It also suggests that if these bars at lookback times of 8-10 Gyr survive out to present epochs, bar-driven secular processes may operate over a long time and have a significant impact on some galaxies by z ~ 0.

Peer Review Status:Awaiting Review

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3. ChinaXiv:202303.05629
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CEERS Epoch 1 NIRCam Imaging: Reduction Methods and Simulations Enabling Early JWST Science Results

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Micaela B. Bagley Steven L. Finkelstein Anton M. Koekemoer Henry C. Ferguson Pablo Arrabal Haro Mark Dickinson Jeyhan S. Kartaltepe Casey Papovich Pablo G. Pérez-González Nor Pirzkal Rachel S. Somerville Christopher N. A. Willmer Guang Yang L. Y. Aaron Yung Adriano Fontana Andrea Grazian Norman A. Grogin Michaela Hirschmann Lisa J. Kewley Allison Kirkpatrick

Abstract： We present the data release and data reduction process for the Epoch 1 NIRCam observations for the Cosmic Evolution Early Release Science Survey (CEERS). These data consist of NIRCam imaging in six broadband filters (F115W, F150W, F200W, F277W, F356W and F444W) and one medium band filter (F410M) over four pointings, obtained in parallel with primary CEERS MIRI observations (Yang et al. in prep). We reduced the NIRCam imaging with the JWST Calibration Pipeline, with custom modifications and reduction steps designed to address additional features and challenges with the data. Here we provide a detailed description of each step in our reduction and a discussion of future expected improvements. Our reduction process includes corrections for known pre-launch issues such as 1/f noise, as well as in-flight issues including snowballs, wisps, and astrometric alignment. Many of our custom reduction processes were first developed with pre-launch simulated NIRCam imaging over the full 10 CEERS NIRCam pointings. We present a description of the creation and reduction of this simulated dataset in the Appendix. We provide mosaics of the real images in a public release, as well as our reduction scripts with detailed explanations to allow users to reproduce our final data products. These represent one of the first official public datasets released from the Directors Discretionary Early Release Science (DD-ERS) program.

Peer Review Status:Awaiting Review

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4. ChinaXiv:202303.07648
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Extensive Lensing Survey of Optical and Near-Infrared Dark Objects (El Sonido): HST H-Faint Galaxies behind 101 Lensing Clusters

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Fengwu Sun Eiichi Egami Pablo G. Pérez-González Ian Smail Karina I. Caputi Franz E. Bauer Timothy D. Rawle Seiji Fujimoto Kotaro Kohno Ugnė Dudzevičiūtė Hakim Atek Matteo Bianconi Scott C. Chapman Francoise Combes Mathilde Jauzac Jean-Baptiste Jolly Anton M. Koekemoer Georgios E. Magdis Giulia Rodighiero Wiphu Rujopakarn

Abstract： We present a Spitzer/IRAC survey of H-faint ($H_{160} \gtrsim 26.4$, $<5\sigma$) sources in 101 lensing cluster fields. Across a CANDELS/Wide-like survey area of $\sim$648 arcmin$^2$ (effectively $\sim$221 arcmin$^2$ in the source plane), we have securely discovered 53 sources in the IRAC Channel-2 band (CH2, 4.5 $\mathrm{\mu m}$; median CH2$=22.46\pm0.11$ AB mag) that lack robust HST/WFC3-IR F160W counterparts. The most remarkable source in our sample, namely ES-009 in the field of Abell 2813, is the brightest H-faint galaxy at 4.5 $\mathrm{\mu m}$ known so far ($\mathrm{CH2}=20.48\pm0.03$ AB mag). We show that the H-faint sources in our sample are massive (median $M_\mathrm{star} = 10^{10.3\pm 0.3}$ $M_\odot$), star-forming (median star formation rate $=100_{-40}^{+60}$ $M_\odot$yr$^{-1}$) and dust-obscured ($A_V=2.6\pm0.3$) galaxies around a median photometric redshift of $z=3.9\pm0.4$. The stellar continua of 14 H-faint galaxies can be resolved in the CH2 band, suggesting a median circularized effective radius ($R_\mathrm{e,circ}$; lensing corrected) of $1.9\pm0.2$ kpc and $<1.5$ kpc for the resolved and whole samples, respectively. This is consistent with the sizes of massive unobscured galaxies at $z\sim4$, indicating that H-faint galaxies represent the dusty tail of the distribution of a wider galaxy population. Comparing with the ALMA dust continuum sizes of similar galaxies reported previously, we conclude that the heavy dust obscuration in H-faint galaxies is related to the compactness of both stellar and dust continua ($R_\mathrm{e,circ}\sim 1$ kpc). These H-faint galaxies make up $16_{-7}^{+13}$% of the galaxies in the stellar mass range of $10^{10}-10^{11.2}$ $M_\odot$ at $z=3\sim5$, contributing to $8_{-4}^{+8}$% of the cosmic star formation rate density in this epoch and likely tracing the early phase of massive galaxy formation.

Peer Review Status:Awaiting Review

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5. ChinaXiv:202303.03680
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The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Micaela B. Bagley Nor Pirzkal Steven L. Finkelstein Casey Papovich Danielle A. Berg Jennifer M. Lotz Gene C. K. Leung Henry C. Ferguson Anton M. Koekemoer Mark Dickinson Jeyhan S. Kartaltepe Dale D. Kocevski Rachel S. Somerville L. Y. Aaron Yung Bren E. Backhaus Caitlin M. Casey Marco Castellano Óscar A. Chávez Ortiz Katherine Chworowsky Isabella G. Cox

Abstract： We present the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey, a deep slitless spectroscopic and imaging Cycle 1 JWST treasury survey designed to constrain feedback mechanisms in low-mass galaxies across cosmic time. NGDEEP targets the Hubble Ultra Deep Field (HUDF) with NIRISS slitless spectroscopy (f~1.2e-18 erg/s/cm^2, 5sigma) to measure metallicities and star-formation rates (SFRs) for low-mass galaxies through the peak of the cosmic SFR density (0.512, constraining the slope of the faint-end of the rest-ultraviolet luminosity function. NGDEEP overlaps with the deepest HST ACS optical imaging in the sky: F435W in the HUDF (m=29.6), and F814W in HUDF-Par2 (m=30), making this a premier HST+JWST Deep Field. As a treasury survey, NGDEEP data is public immediately, and we will rapidly release data products and catalogs in the spirit of previous deep field initiatives. In this paper we present the NGDEEP survey design, summarize the science goals, and detail plans for the public release of NGDEEP reduced data products.

Peer Review Status:Awaiting Review

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6. ChinaXiv:202303.03570
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ALMA FIR View of Ultra High-redshift Galaxy Candidates at $z\sim$ 11-17: Blue Monsters or Low-$z$ Red Interlopers?

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Seiji Fujimoto Steven L. Finkelstein Denis Burgarella Chris L. Carilli Véronique Buat Caitlin M. Casey Laure Ciesla Sandro Tacchella Jorge A. Zavala Gabriel Brammer Yoshinobu Fudamoto Masami Ouchi Francesco Valentino M. C. Cooper Mark Dickinson Maximilien Franco Mauro Giavalisco Taylor A. Hutchison Jeyhan S. Kartaltepe Anton M. Koekemoer

Abstract： We present ALMA Band 7 observations of a remarkably bright galaxy candidate at $z_{\rm phot}$=$16.7^{+1.9}_{-0.3}$ ($M_{\rm UV}$=$-21.6$), S5-z17-1, identified in JWST Early Release Observation data of Stephen's Quintet. We do not detect the dust continuum at 866 $\mu$m, ruling out the possibility that S5-z17-1 is a low-$z$ dusty starburst with a star-formation rate (SFR) of $\gtrsim 30\,M_{\odot}$ yr$^{-1}$. We detect a 5.1$\sigma$ line feature at $338.726\pm0.007$ GHz exactly coinciding with the JWST source position, with a 2% likelihood of the signal being spurious. The most likely line identification would be [OIII]52$\mu$m at $z=16.01$ or [CII]158$\mu$m at $z=4.61$, whose line luminosities do not violate the non-detection of the dust continuum in both cases. Together with three other $z\gtrsim$ 11-13 candidate galaxies recently observed with ALMA, we conduct a joint ALMA and JWST spectral energy distribution (SED) analysis and find that the high-$z$ solution at $z\sim$11-17 is favored in every candidate as a very blue (UV continuum slope of $\approx-2.3$) and luminous ($M_{\rm UV}$ $\approx$ [$-$24:$-$21]) system. Still, we find in some candidates that reasonable SED fits ($\Delta$ $\chi^{2}\lesssim4$) are reproduced by type-II quasar and/or quiescent galaxy templates with strong emission lines at $z\sim3$-5, where such populations predicted from their luminosity functions and EW([OIII]+H$\beta$) distributions are abundant in survey volumes used for the $z\sim$11-17 candidates. While these recent ALMA observation results have strengthened the likelihood of the high-$z$ solutions, lower-$z$ possibilities are not completely ruled out in some of the $z\sim$11-17 candidates.

Peer Review Status:Awaiting Review

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7. ChinaXiv:202303.05906
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ALMA Lensing Cluster Survey: ALMA-Herschel Joint Study of Lensed Dusty Star-Forming Galaxies across $z\simeq0.5-6$

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Fengwu Sun Eiichi Egami Seiji Fujimoto Timothy Rawle Franz E. Bauer Kotaro Kohno Ian Smail Pablo G. Pérez-González Yiping Ao Scott C. Chapman Francoise Combes Miroslava Dessauges-Zavadsky Daniel Espada Jorge González-López Anton M. Koekemoer Vasily Kokorev Minju M. Lee Kana Morokuma-Matsui Alejandra M. Muñoz Arancibia Masamune Oguri

Abstract： We present an ALMA-Herschel joint analysis of sources detected by the ALMA Lensing Cluster Survey (ALCS) at 1.15 mm. Herschel/PACS and SPIRE data at 100-500 $\mu$m are deblended for 180 ALMA sources in 33 lensing cluster fields that are either detected securely (141 sources; in our main sample) or tentatively at S/N$\geq$4 with cross-matched HST/Spitzer counterparts, down to a delensed 1.15-mm flux density of $\sim0.02$ mJy. We performed far-infrared spectral energy distribution modeling and derived the physical properties of dusty star formation for 125 sources (109 independently) that are detected at $>2\sigma$ in at least one Herschel band. 27 secure ALCS sources are not detected in any Herschel bands, including 17 optical/near-IR-dark sources that likely reside at $z=4.2\pm1.2$. The 16-50-84 percentiles of the redshift distribution are 1.15-2.08-3.59 for ALCS sources in the main sample, suggesting an increasing fraction of $z\simeq1-2$ galaxies among fainter millimeter sources ($f_{1150}\sim 0.1$ mJy). With a median lensing magnification factor of $\mu = 2.6_{-0.8}^{+2.6}$, ALCS sources in the main sample exhibit a median intrinsic star-formation rate of $94_{-54}^{+84}\,\mathrm{M}_\odot\,\mathrm{yr}^{-1}$, lower than that of conventional submillimeter galaxies at similar redshifts by a factor of $\sim$3. Our study suggests weak or no redshift evolution of dust temperature with $L_\mathrm{IR}<10^{12}\,\mathrm{L}_\odot$ galaxies within our sample at $z \simeq 0 - 2$. At $L_\mathrm{IR}>10^{12}\,\mathrm{L}_\odot$, the dust temperatures show no evolution across $z \simeq 1 -4$ while being lower than those in the local Universe. For the highest-redshift source in our sample ($z=6.07$), we can rule out an extreme dust temperature ($>$80 K) that was reported for MACS0416 Y1 at $z=8.31$.

Peer Review Status:Awaiting Review

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8. ChinaXiv:202303.03324
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CEERS Key Paper V: A triality on the nature of HST-dark galaxies

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Pablo G. Pérez-González Guillermo Barro Marianna Annunziatella Luca Costantin Ángela García-Argumánez Elizabeth J. McGrath Rosa M. Mérida Jorge A. Zavala Pablo Arrabal Haro Micaela B. Bagley Bren E. Backhaus Peter Behroozi Eric F. Bell Véronique Buat Antonello Calabrò Caitlin M. Casey Nikko J. Cleri Rosemary T. Coogan M. C. Cooper Asantha R. Cooray

Abstract： The new capabilities that JWST offers in the near- and mid-infrared (IR) are used to investigate in unprecedented detail the nature of optical/near-IR faint, mid-IR bright sources, HST-dark galaxies among them. We gather JWST data from the CEERS survey in the EGS, jointly with HST data, and analyze spatially resolved optical-to-mid-IR spectral energy distributions (SEDs) to estimate both photometric redshifts in 2 dimensions and stellar populations properties in a pixel-by-pixel basis. We select 138 galaxies with F150W-F356W>1.5 mag, F356W<27.5 mag. The nature of these sources is threefold: (1) 71% are dusty star-forming galaxies at 2100 Gyr^-1); (2) 18% are quiescent/dormant (i.e., subject to reignition and rejuvenation) galaxies at 3展开 -->

Peer Review Status:Awaiting Review

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9. ChinaXiv:202303.03385
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CEERS Key Paper IV: Galaxies at $4 < z < 9$ are Bluer than They Appear -- Characterizing Galaxy Stellar Populations from Rest-Frame $\sim 1$ micron Imaging

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Casey Papovich Justin Cole Guang Yang Steven L. Finkelstein Guillermo Barro Véronique Buat Denis Burgarella Pablo G. Pérez-González Paola Santini Lise-Marie Seillé Lu Shen Pablo Arrabal Haro Micaela B. Bagley Eric F. Bell Laura Bisigello Antonello Calabrò Caitlin M. Casey Marco Castellano Katherine Chworowsky Nikko J. Cleri

Abstract： We present results from the Cosmic Evolution Early Release Survey (CEERS) on the stellar-population parameters for 28 galaxies with redshifts $4展开 -->

Peer Review Status:Awaiting Review

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10. ChinaXiv:202303.06427
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Implications of Increased Central Mass Surface Densities for the Quenching of Low-mass Galaxies

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Yicheng Guo Timothy Carleton Eric F. Bell Zhu Chen Avishai Dekel S. M. Faber Mauro Giavalisco Dale D. Kocevski Anton M. Koekemoer David C. Koo Peter Kurczynski Seong-Kook Lee F. S. Liu Casey Papovich Pablo G. Pérez-González

Abstract： We use the Cosmic Assembly Deep Near-infrared Extragalactic Legacy Survey (CANDELS) data to study the relationship between quenching and the stellar mass surface density within the central radius of 1 kpc ($\Sigma_1$) of low-mass galaxies (stellar mass $M_* \lesssim 10^{9.5} M_\odot$) at $0.5 \leq z < 1.5$. Our sample is mass complete down to $\sim 10^9 M_\odot$ at $0.5 \leq z < 1.0$. We compare the mean $\Sigma_1$ of star-forming galaxies (SFGs) and quenched galaxies (QGs) at the same redshift and $M_*$. We find that low-mass QGs have higher $\Sigma_1$ than low-mass SFGs, similar to galaxies above $10^{10} M_\odot$. The difference of $\Sigma_1$ between QGs and SFGs increases slightly with $M_*$ at $M_* \lesssim 10^{10} M_\odot$ and decreases with $M_*$ at $M_* \gtrsim 10^{10} M_\odot$. The turnover mass is consistent with the mass where quenching mechanisms transition from internal to environmental quenching. At $0.5 \leq z < 1.0$, we find that the $\Sigma_1$ of galaxies increases by about 0.25 dex in the green valley (i.e., the transitioning region from star forming to fully quenched), regardless of their $M_*$. Using the observed specific star formation rate (sSFR) 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 ($\sim4$) Gyrs at $0.5 \leq z < 1.0$. 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 $\Sigma_1$. An interesting and intriguing result is the similarity of the growth of $\Sigma_1$ 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.

Peer Review Status:Awaiting Review

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11. ChinaXiv:202303.02766
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A z=1.85 galaxy group in CEERS: evolved, dustless, massive Intra-Halo Light and a Brightest Group Galaxy in the making

Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19

Rosemary T. Coogan Emanuele Daddi Aurélien Le Bail David Elbaz Mark Dickinson Mauro Giavalisco Carlos Gómez-Guijarro Alexander de la Vega Micaela Bagley Steven L. Finkelstein Maximilien Franco Asantha R. Cooray Peter Behroozi Laura Bisigello Caitlin M. Casey Laure Ciesla Paola Dimauro Alexis Finoguenov Anton M. Koekemoer Ray A. Lucas

Abstract： We present CEERS JWST/NIRCam imaging of a massive galaxy group at z=1.85, to explore the early JWST view on massive group formation in the distant Universe. The group contains >16 members (including 6 spectros. confirmations) down to log10(Mstar/Msun)=8.5, including the Brightest Group Galaxy (BGG) in the process of actively assembling at this redshift. The BGG is comprised of multiple merging components extending ~3.6" (30kpc) across the sky. The BGG contributes 69% of the group's total galactic stellar mass, with one of the merging components containing 76% of the total mass of the BGG and a SFR>1810Msun/yr. Most importantly, we detect intra-halo light (IHL) in several HST and JWST/NIRCam bands, allowing us to construct a state-of-the-art rest-frame UV-NIR Spectral Energy Distribution of the IHL for the first time at this high redshift. This allows stellar population characterisation of both the IHL and member galaxies, as well as the morphology distribution of group galaxies vs. their star-formation activity when coupled with Herschel data. We create a stacked image of the IHL, giving us a sensitivity to extended emission of 28.5 mag/arcsec2 at rest-frame 1um. We find that the IHL is extremely dust poor (Av~0), containing an evolved stellar population of log10(t50/yr)=8.8, corresponding to a formation epoch for 50% of the stellar material 0.63Gyr before z=1.85. There is no evidence of ongoing star-formation in the IHL. The IHL in this group at z=1.85 contributes ~10% of the total stellar mass, comparable with what is observed in local clusters. This suggests that the evolution of the IHL fraction is more self-similar with redshift than predicted by some models, challenging our understanding of IHL formation during the assembly of high-redshift clusters. JWST is unveiling a new side of group formation at this redshift, which will evolve into Virgo-like structures in the local Universe.

Peer Review Status:Awaiting Review

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