Search

Your search keyword '"Hathi, NP"' showing total 23 results
Start Over Author "Hathi, NP"
23 results on '"Hathi, NP"'

1. Spectroscopy of the supernova H0pe host galaxy at redshift 1.78

Author

Polletta, M, Nonino, M, Frye, B, Gargiulo, A, Bisogni, S, Garuda, N, Thompson, D, Lehnert, M, Pascale, M, Willner, SP, Kamieneski, P, Leimbach, R, Cheng, C, Coe, D, Cohen, SH, Conselice, CJ, Dai, L, Diego, J, Dole, H, Driver, SP, D’Silva, JCJ, Fontana, A, Foo, N, Furtak, LJ, Grogin, NA, Harrington, K, Hathi, NP, Jansen, RA, Kelly, P, Koekemoer, AM, Mancini, C, Marshall, MA, Pierel, JDR, Pirzkal, N, Robotham, A, Rutkowski, MJ, Ryan, RE, Snigula, JM, Summers, J, Tompkins, S, Willmer, CNA, Windhorst, RA, Yan, H, Yun, MS, and Zitrin, A

Subjects
Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

Supernova (SN) H0pe was discovered as a new transient in James Webb Space Telescope (JWST) NIRCam images of the galaxy cluster PLCK G165.7+67.0 taken as part of the Prime Extragalactic Areas for Reionization and Lensing Science (PEARLS) JWST GTO program (ID 1176) on 2023 March 30. The transient is a compact source associated with a background galaxy that is stretched and triply imaged by the strong gravitational lensing of the cluster. This paper reports spectra in the 950- 1370 nm observer frame of two of the galaxy images obtained with Large Binocular Telescope (LBT) Utility Camera in the Infrared (LUCI) in long-slit mode two weeks after the JWST observations. The individual and average spectra show the [O′ ¯II] λλ3727,3730 doublet and the Balmer and 4000 Åbreaks at redshift z = 1.783 ± 0.002. The code investigating galaxy emission (CIGALE) best-fit model of the spectral energy distribution indicates that the host galaxy of SN H0pe is massive (Mstar ≃ 6 × 1010 M⊙ after correcting for a magnification factor μ ~ 7) with a predominantly intermediate-age (~2 Gyr) stellar population, moderate extinction, and a magnification-corrected star formation rate ≃13 M⊙ yr-1, consistent with being below the main sequence of star formation. These properties suggest that H0pe might be a type Ia SN. Additional observations of SN H0pe and its host recently carried out with JWST (JWST-DD-4446; PI: B. Frye) will be able to both determine the SN classification and confirm its association with the galaxy analyzed in this work.

Published
2023

2. The size and pervasiveness of Ly α-UV spatial offsets in star-forming galaxies at z ∼6

Author

Lemaux, BC, Fuller, S, Bradač, M, Pentericci, L, Hoag, A, Strait, V, Treu, T, Alvarez, C, Bolan, P, Gandhi, PJ, Huang, KH, Jones, T, Mason, C, Pelliccia, D, Ribeiro, B, Ryan, RE, Schmidt, KB, Vanzella, E, Khusanova, Y, Le Fèvre, O, Guaita, L, Hathi, NP, Koekemoer, A, and Pforr, J

Subjects
gravitational lensing: strong, techniques: photometric, techniques: spectroscopic, galaxies: evolution, galaxies: high-redshift, reionization, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We study the projected spatial offset between the ultraviolet continuum and Ly α emission for 65 lensed and unlensed galaxies in the Epoch of Reionization (5 ≤ z ≤ 7), the first such study at these redshifts, in order to understand the potential for these offsets to confuse estimates of the Ly α properties of galaxies observed in slit spectroscopy. While we find that ∼40 per cent of galaxies in our sample show significant projected spatial offsets ($|\Delta {\rm {Ly}\alpha -\rm {UV}}|$), we find a relatively modest average projected offset of $|\widetilde{\Delta }{\rm {Ly}\alpha -\rm {UV}}|$ = 0.61 ± 0.08 proper kpc for the entire sample. A small fraction of our sample, ∼10 per cent, exhibit offsets in excess of 2 proper kpc, with offsets seen up to ∼4 proper kpc, sizes that are considerably larger than the effective radii of typical galaxies at these redshifts. An internal comparison and a comparison to studies at lower redshift yielded no significant evidence of evolution of $|\Delta {\rm {Ly}\alpha -\rm {UV}}|$ with redshift. In our sample, ultraviolet (UV)-bright galaxies ($\widetilde{L{\mathrm{ UV}}}/L{\ast }{\mathrm{ UV}}=0.67$) showed offsets a factor of three greater than their fainter counterparts ($\widetilde{L{\mathrm{ UV}}}/L{\ast }{\mathrm{ UV}}=0.10$), 0.89 ± 0.18 versus 0.27 ± 0.05 proper kpc, respectively. The presence of companion galaxies and early stage merging activity appeared to be unlikely causes of these offsets. Rather, these offsets appear consistent with a scenario in which internal anisotropic processes resulting from stellar feedback, which is stronger in UV-brighter galaxies, facilitate Ly α fluorescence and/or backscattering from nearby or outflowing gas. The reduction in the Ly α flux due to offsets was quantified. It was found that the differential loss of Ly α photons for galaxies with average offsets is not, if corrected for, a limiting factor for all but the narrowest slit widths (

Published
2021

3. An Ultra Deep Field survey with WFIRST

Author

Koekemoer, Anton M, Foley, RJ, Spergel, DN, Bagley, M, Bezanson, R, Bianco, FB, Bouwens, R, Bradley, L, Brammer, G, Capak, P, Davidzon, I, Rosa, G De, Dickinson, ME, Doré, O, Dunlop, JS, Ellis, RS, Fan, X, Fazio, GG, Ferguson, HC, Filippenko, AV, Finkelstein, S, Frye, B, Gawiser, E, Grogin, NA, Hathi, NP, Hirata, CM, Hounsell, R, Illingworth, GD, Jansen, RA, Jauzac, M, Jha, SW, Kartaltepe, JS, Kim, AG, Kelly, P, Kruk, JW, Larson, R, Lotz, J, Lucas, R, Malhotra, S, Mandel, K, Margutti, R, Marrone, D, McLure, RJ, McQuinn, K, Melchior, P, Mobasher, B, Mould, JR, Moustakas, L, Newman, JA, Papovich, C, Peeples, MS, Perlmutter, S, Pirzkal, N, Rhoads, J, Rhodes, J, Robertson, B, Rubin, D, Ryan, R, Scolnic, D, Shapley, A, Somerville, R, Steinhardt, C, Stiavelli, M, Street, R, Trenti, M, Treu, T, Wang, L, Wang, Y, Whalen, D, Windhorst, RA, Wollack, EJ, and Yan, H

Subjects
astro-ph.GA
Abstract

Studying the formation and evolution of galaxies at the earliest cosmictimes, and their role in reionization, requires the deepest imaging possible.Ultra-deep surveys like the HUDF and HFF have pushed to mag \mAB$\,\sim\,$30,revealing galaxies at the faint end of the LF to $z$$\,\sim\,$9$\,-\,$11 andconstraining their role in reionization. However, a key limitation of thesefields is their size, only a few arcminutes (less than a Mpc at theseredshifts), too small to probe large-scale environments or clusteringproperties of these galaxies, crucial for advancing our understanding ofreionization. Achieving HUDF-quality depth over areas $\sim$100 times largerbecomes possible with a mission like the Wide Field Infrared Survey Telescope(WFIRST), a 2.4-m telescope with similar optical properties to HST, with afield of view of $\sim$1000 arcmin$^2$, $\sim$100$\times$ the area of theHST/ACS HUDF. This whitepaper motivates an Ultra-Deep Field survey with WFIRST, covering$\sim$100$\,-\,$300$\times$ the area of the HUDF, or up to $\sim$1 deg$^2$, to\mAB$\,\sim\,$30, potentially revealing thousands of galaxies and AGN at thefaint end of the LF, at or beyond $z$\,$\sim$\,9$\,-\,$10 in the epoch ofreionization, and tracing their LSS environments, dramatically increasing thediscovery potential at these redshifts. (Note: This paper is a somewhat expanded version of one that was submitted asinput to the Astro2020 Decadal Survey, with this version including an Appendix(which exceeded the Astro2020 page limits), describing how the science driversfor a WFIRST Ultra Deep Field might map into a notional observing program,including the filters used and exposure times needed to achieve these depths.)

Published
2019

4. LSST Observing Strategy White Paper: LSST Observations of WFIRST Deep Fields

Author

Foley, RJ, Koekemoer, AM, Spergel, DN, Bianco, FB, Capak, P, Dai, L, Dore, O, Fazio, GG, Ferguson, H, Filippenko, AV, Frye, B, Galbany, L, Gawiser, E, Gronwall, C, Hathi, NP, Hirata, C, Hounsell, R, Jha, SW, Kim, AG, Kelly, PL, Kruk, JW, Malhotra, S, Mandel, KS, Margutti, R, Marrone, D, McQuinn, KBW, Melchior, P, Moustakas, L, Newman, JA, Peek, JEG, Perlmutter, S, Rhodes, JD, Robertson, B, Rubin, D, Scolnic, D, Somerville, R, Street, R, Wang, Y, Whalen, DJ, Windhorst, RA, and Wollack, EJ

Subjects
astro-ph.IM, astro-ph.GA
Abstract

The Wide-Field Infrared Survey Telescope (WFIRST) is expected to launch inthe mid-2020s. With its wide-field near-infrared (NIR) camera, it will surveythe sky to unprecedented detail. As part of normal operations and as the resultof multiple expected dedicated surveys, WFIRST will produce several relativelywide-field (tens of square degrees) deep (limiting magnitude of 28 or fainter)fields. In particular, a planned supernova survey is expected to image 3 deepfields in the LSST footprint roughly every 5 days over 2 years. Stacking alldata, this survey will produce, over all WFIRST supernova fields in the LSSTfootprint, ~12-25 deg^2 and ~5-15 deg^2 regions to depths of ~28 mag and ~29mag, respectively. We suggest LSST undertake mini-surveys that will match theWFIRST cadence and simultaneously observe the supernova survey fields duringthe 2-year WFIRST supernova survey, achieving a stacked depth similar to thatof the WFIRST data. We also suggest additional observations of these sameregions throughout the LSST survey to get deep images earlier, have long-termmonitoring in the fields, and produce deeper images overall. These fields willprovide a legacy for cosmology, extragalactic, and transient/variable science.

Published
2018

5. STELLAR MASS-GAS-PHASE METALLICITY RELATION at 0.5 ≤ z ≤ 0.7: A POWER LAW with INCREASING SCATTER TOWARD the LOW-MASS REGIME

Author

Guo, Y, Koo, DC, Lu, Y, Forbes, JC, Rafelski, M, Trump, JR, Amorín, R, Barro, G, Davé, R, Faber, SM, Hathi, NP, Yesuf, H, Cooper, MC, Dekel, A, Guhathakurta, P, Kirby, EN, Koekemoer, AM, Pérez-González, PG, Lin, L, Newman, JA, Primack, JR, Rosario, DJ, Willmer, CNA, and Yan, R

Subjects
galaxies: abundances, galaxies: dwarf, galaxies: evolution, galaxies: formation, galaxies: fundamental parameters, galaxies: ISM, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We present the stellar mass (M∗)gas-phase metallicity relation (MZR) and its scatter at intermediate redshifts (0.5 ≤ z ≤ 0.7) for 1381 field galaxies collected from deep spectroscopic surveys. The star formation rate (SFR) and color at a given M∗ of this magnitude-limited (R ≳ 24 AB) sample are representative of normal starforming galaxies. For masses below 109 Mo, our sample of 237 galaxies is ∼10 times larger than those in previous studies beyond the local universe. This huge gain in sample size enables superior constraints on the MZR and its scatter in the low-mass regime. We find a power-law MZR at 108 Mo < M∗ < 1011 Mo: 12 + log (O/H) = (5.83 ± 0.19) +(0.30 ± 0.02) log (M∗/Mo). At 109 Mo < M∗ < 1010.5 Mo, our MZR shows agreement with others measured at similar redshifts in the literature. Our power-law slope is, however, shallower than the extrapolation of the MZRs of others to masses below 109 Mo. The SFR dependence of the MZR in our sample is weaker than that found for local galaxies (known as the fundamental metallicity relation). Compared to a variety of theoretical models, the slope of our MZR for low-mass galaxies agrees well with predictions incorporating supernova energy-driven winds. Being robust against currently uncertain metallicity calibrations, the scatter of the MZR serves as a powerful diagnostic of the stochastic history of gas accretion, gas recycling, and star formation of low-mass galaxies. Our major result is that the scatter of our MZR increases as Mo decreases. Our result implies that either the scatter of the baryonic accretion rate (δṀ? ) or the scatter of the M∗-Mhalo relation (δSHMR) increases as M∗ decreases. Moreover, our measure of scatter at z = 0.7 appears consistent with that found for local galaxies. This lack of redshift evolution constrains models of galaxy evolution to have both δṀ and δSHMR remain unchanged from z = 0.7 to z = 0.

Published
2016

6. STELLAR MASSES FROM THE CANDELS SURVEY: THE GOODS-SOUTH AND UDS FIELDS

Author

Santini, P, Ferguson, HC, Fontana, A, Mobasher, B, Barro, G, Castellano, M, Finkelstein, SL, Grazian, A, Hsu, LT, Lee, B, Lee, S-K, Pforr, J, Salvato, M, Wiklind, T, Wuyts, S, Almaini, O, Cooper, MC, Galametz, A, Weiner, B, Amorin, R, Boutsia, K, Conselice, CJ, Dahlen, T, Dickinson, ME, Giavalisco, M, Grogin, NA, Guo, Y, Hathi, NP, Kocevski, D, Koekemoer, AM, Kurczynski, P, Merlin, E, Mortlock, A, Newman, JA, Paris, D, Pentericci, L, Simons, R, and Willner, SP

Subjects
Space Sciences, Physical Sciences, catalogs, galaxies: fundamental parameters, galaxies: high-redshift, galaxies: stellar content, surveys, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present the public release of the stellar mass catalogs for the GOODS-S and UDS fields obtained using some of the deepest near-IR images available, achieved as part of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey project. We combine the effort from 10 different teams, who computed the stellar masses using the same photometry and the same redshifts. Each team adopted their preferred fitting code, assumptions, priors, and parameter grid. The combination of results using the same underlying stellar isochrones reduces the systematics associated with the fitting code and other choices. Thanks to the availability of different estimates, we can test the effect of some specific parameters and assumptions on the stellar mass estimate. The choice of the stellar isochrone library turns out to have the largest effect on the galaxy stellar mass estimates, resulting in the largest distributions around the median value (with a semi interquartile range larger than 0.1 dex). On the other hand, for most galaxies, the stellar mass estimates are relatively insensitive to the different parameterizations of the star formation history. The inclusion of nebular emission in the model spectra does not have a significant impact for the majority of galaxies (less than a factor of 2 for 80% of the sample). Nevertheless, the stellar mass for the subsample of young galaxies (age

Published
2015

7. Physical properties of emission-line galaxies at z ∼ 2 from near-infrared spectroscopy with magellan fire

Author

Masters, D, McCarthy, P, Siana, B, Malkan, M, Mobasher, B, Atek, H, Henry, A, Martin, CL, Rafelski, M, Hathi, NP, Scarlata, C, Ross, NR, Bunker, AJ, Blanc, G, Bedregal, AG, Domínguez, A, Colbert, J, Teplitz, H, and Dressler, A

Subjects
galaxies: abundances, galaxies: high-redshift, galaxies: kinematics and dynamics, galaxies: starburst, galaxies: star formation, astro-ph.GA, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We present results from near-infrared spectroscopy of 26 emission-line galaxies at z ∼ 2.2 and z ∼ 1.5 obtained with the Folded-port InfraRed Echellette (FIRE) spectrometer on the 6.5 m Magellan Baade telescope. The sample was selected from the WFC3 Infrared Spectroscopic Parallels survey, which uses the near-infrared grism of the Hubble Space Telescope Wide Field Camera 3 (WFC3) to detect emission-line galaxies over 0.3 ≲ z ≲ 2.3. Our FIRE follow-up spectroscopy (R ∼ 5000) over 1.0-2.5 μm permits detailed measurements of the physical properties of the z ∼ 2 emission-line galaxies. Dust-corrected star formation rates for the sample range from ∼5-100 MȮ yr-1 with a mean of 29 MȮ yr-1. We derive a median metallicity for the sample of 12 + log(O/H) = 8.34 or ∼0.45 ZȮ. The estimated stellar masses range from ∼108.5-109.5 MȮ, and a clear positive correlation between metallicity and stellar mass is observed. The average ionization parameter measured for the sample, log U ≈ -2.5, is significantly higher than what is found for most star-forming galaxies in the local universe, but similar to the values found for other star-forming galaxies at high redshift. We derive composite spectra from the FIRE sample, from which we measure typical nebular electron densities of ∼100-400 cm-3. Based on the location of the galaxies and composite spectra on diagnostic diagrams, we do not find evidence for significant active galactic nucleus activity in the sample. Most of the galaxies, as well as the composites, are offset diagram toward higher [O III]/Hβ at a given [N II]/Hα, in agreement with other observations of z ≳ 1 star-forming galaxies, but composite spectra derived from the sample do not show an appreciable offset from the local star-forming sequence on the [O III]/Hβ versus [S II]/Hα diagram. We infer a high nitrogen-to-oxygen abundance ratio from the composite spectrum, which may contribute to the offset of the high-redshift galaxies from the local star-forming sequence in the [O III]/Hβ versus [N II]/Hα diagram. We speculate that the elevated nitrogen abundance could result from substantial numbers of Wolf-Rayet stars in starbursting galaxies at z ∼ 2. © 2014. The American Astronomical Society. All rights reserved.

Published
2014

8. HST/WFC3 NEAR-INFRARED SPECTROSCOPY OF QUENCHED GALAXIES AT z ∼ 1.5 FROM THE WISP SURVEY: STELLAR POPULATION PROPERTIES**Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555.

Author

Bedregal, AG, Scarlata, C, Henry, AL, Atek, H, Rafelski, M, Teplitz, HI, Dominguez, A, Siana, B, Colbert, JW, Malkan, M, Ross, NR, Martin, CL, Dressler, A, Bridge, C, Hathi, NP, Masters, D, McCarthy, PJ, and Rutkowski, MJ

Subjects
galaxies: formation, galaxies: high-redshift, galaxies: stellar content, Galaxy: evolution, nfrared: galaxies, surveys, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We combine Hubble Space Telescope (HST) G102 and G141 near-IR (NIR) grism spectroscopy with HST/WFC3-UVIS, HST/WFC3-IR, and Spitzer/IRAC [3.6 μm] photometry to assemble a sample of massive (log (M star/M ⊙) ∼ 11.0) and quenched (specific star formation rate 2 and the z ∼ 1.5 RS. According to their estimated ages, the time required for quenched galaxies off the RS to join their counterparts on the z ∼ 1.5 RS is of the order of ∼1 Gyr. © 2013. The American Astronomical Society. All rights reserved.

Published
2013

9. Dusty Starbursts Masquerading as Ultra-high Redshift Galaxies in JWST CEERS Observations

Author

Zavala, JA, Buat, V, Casey, CM, Finkelstein, SL, Burgarella, D, Bagley, MB, Ciesla, L, Daddi, E, Dickinson, M, Ferguson, HC, Franco, M, Jiménez-Andrade, EF, Kartaltepe, JS, Koekemoer, AM, Bail, AL, Murphy, EJ, Papovich, C, Tacchella, S, Wilkins, SM, Aretxaga, I, Behroozi, P, Champagne, JB, Fontana, A, Giavalisco, M, Grazian, A, Grogin, NA, Kewley, LJ, Kocevski, DD, Kirkpatrick, A, Lotz, JM, Pentericci, L, Pérez-González, PG, Pirzkal, N, Ravindranath, S, Somerville, RS, Trump, Yang, G, Aaron Yung, LY, Almaini, O, Amorín, RO, Annunziatella, M, Haro, PA, Backhaus, BE, Barro, G, Bell, EF, Bhatawdekar, R, Bisigello, L, Buitrago, F, Calabrò, A, Castellano, M, Chávez Ortiz, ÓA, Chworowsky, K, Cleri, NJ, Cohen, SH, Cole, JW, Cooke, KC, Cooper, MC, Cooray, AR, Costantin, L, Cox, IG, Croton, D, Davé, R, Vega, ADL, Dekel, A, Elbaz, D, Estrada-Carpenter, V, Fernández, V, Finkelstein, KD, Freundlich, J, Fujimoto, S, García-Argumánez, Á, Gardner, JP, Gawiser, E, Gómez-Guijarro, C, Guo, Y, Hamilton, TS, Hathi, NP, Holwerda, BW, Hirschmann, M, Huertas-Company, M, Hutchison, TA, Iyer, KG, Jaskot, AE, Jha, SW, Jogee, S, Juneau, S, Jung, I, Kassin, SA, Kurczynski, P, Larson, RL, Leung, GCK, Long, AS, Lucas, RA, Magnelli, B, Mantha, KB, Matharu, J, McGrath, EJ, McIntosh, DH, Medrano, A, Merlin, E, Zavala, JA [0000-0002-7051-1100], Buat, V [0000-0003-3441-903X], Casey, CM [0000-0002-0930-6466], Finkelstein, SL [0000-0001-8519-1130], Burgarella, D [0000-0002-4193-2539], Bagley, MB [0000-0002-9921-9218], Ciesla, L [0000-0003-0541-2891], Daddi, E [0000-0002-3331-9590], Dickinson, M [0000-0001-5414-5131], Ferguson, HC [0000-0001-7113-2738], Franco, M [0000-0002-3560-8599], Jiménez-Andrade, EF [0000-0002-2640-5917], Kartaltepe, JS [0000-0001-9187-3605], Koekemoer, AM [0000-0002-6610-2048], Bail, AL [0000-0002-9466-2763], Murphy, EJ [0000-0001-7089-7325], Papovich, C [0000-0001-7503-8482], Tacchella, S [0000-0002-8224-4505], Wilkins, SM [0000-0003-3903-6935], Aretxaga, I [0000-0002-6590-3994], Behroozi, P [0000-0002-2517-6446], Champagne, JB [0000-0002-6184-9097], Fontana, A [0000-0003-3820-2823], Giavalisco, M [0000-0002-7831-8751], Grazian, A [0000-0002-5688-0663], Grogin, NA [0000-0001-9440-8872], Kewley, LJ [0000-0001-8152-3943], Kocevski, DD [0000-0002-8360-3880], Kirkpatrick, A [0000-0002-5537-8110], Lotz, JM [0000-0003-3130-5643], Pentericci, L [0000-0001-8940-6768], Pérez-González, PG [0000-0003-4528-5639], Pirzkal, N [0000-0003-3382-5941], Ravindranath, S [0000-0002-5269-6527], Somerville, RS [0000-0002-6748-6821], Trump, JR [0000-0002-1410-0470], Yang, G [0000-0001-8835-7722], Aaron Yung, LY [0000-0003-3466-035X], Almaini, O [0000-0001-9328-3991], Amorín, RO [0000-0001-5758-1000], Annunziatella, M [0000-0002-8053-8040], Haro, PA [0000-0002-7959-8783], Backhaus, BE [0000-0001-8534-7502], Barro, G [0000-0001-6813-875X], Bell, EF [0000-0002-5564-9873], Bhatawdekar, R [0000-0003-0883-2226], Bisigello, L [0000-0003-0492-4924], Buitrago, F [0000-0002-2861-9812], Calabrò, A [0000-0003-2536-1614], Castellano, M [0000-0001-9875-8263], Chávez Ortiz, ÓA [0000-0003-2332-5505], Chworowsky, K [0000-0003-4922-0613], Cleri, NJ [0000-0001-7151-009X], Cohen, SH [0000-0003-3329-1337], Cole, JW [0000-0002-6348-1900], Cooke, KC [0000-0002-2200-9845], Cooper, MC [0000-0003-1371-6019], Cooray, AR [0000-0002-3892-0190], Costantin, L [0000-0001-6820-0015], Cox, IG [0000-0002-1803-794X], Croton, D [0000-0002-5009-512X], Davé, R [0000-0003-2842-9434], Vega, ADL [0000-0002-6219-5558], Dekel, A [0000-0003-4174-0374], Elbaz, D [0000-0002-7631-647X], Estrada-Carpenter, V [0000-0001-8489-2349], Fernández, V [0000-0003-0531-5450], Finkelstein, KD [0000-0003-0792-5877], Freundlich, J [0000-0002-5245-7796], Fujimoto, S [0000-0001-7201-5066], García-Argumánez, Á [0000-0002-8365-5525], Gardner, JP [0000-0003-2098-9568], Gawiser, E [0000-0003-1530-8713], Gómez-Guijarro, C [0000-0002-4085-9165], Guo, Y [0000-0002-4162-6523], Hamilton, TS [0000-0002-9753-1769], Hathi, NP [0000-0001-6145-5090], Holwerda, BW [0000-0002-4884-6756], Hirschmann, M [0000-0002-3301-3321], Huertas-Company, M [0000-0002-1416-8483], Hutchison, TA [0000-0001-6251-4988], Iyer, KG [0000-0001-9298-3523], Jaskot, AE [0000-0002-6790-5125], Jha, SW [0000-0001-8738-6011], Jogee, S [0000-0002-1590-0568], Juneau, S [0000-0002-0000-2394], Jung, I [0000-0003-1187-4240], Kassin, SA [0000-0002-3838-8093], Kurczynski, P [0000-0002-8816-5146], Larson, RL [0000-0003-2366-8858], Leung, GCK [0000-0002-9393-6507], Long, AS [0000-0002-7530-8857], Lucas, RA [0000-0003-1581-7825], Magnelli, B [0000-0002-6777-6490], Matharu, J [0000-0002-7547-3385], McGrath, EJ [0000-0001-8688-2443], Merlin, E [0000-0001-6870-8900], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, 5109 Space Sciences, 51 Physical Sciences, Galaxies and Cosmology
Abstract

Lyman-break galaxy (LBG) candidates at z ≳ 10 are rapidly being identified in James Webb Space Telescope (JWST)/NIRCam observations. Due to the (redshifted) break produced by neutral hydrogen absorption of rest-frame UV photons, these sources are expected to drop out in the bluer filters while being well detected in redder filters. However, here we show that dust-enshrouded star-forming galaxies at lower redshifts (z ≲ 7) may also mimic the near-infrared (near-IR) colors of z > 10 LBGs, representing potential contaminants in LBG candidate samples. First, we analyze CEERS-DSFG-1, a NIRCam dropout undetected in the F115W and F150W filters but detected at longer wavelengths. Combining the JWST data with (sub)millimeter constraints, including deep NOEMA interferometric observations, we show that this source is a dusty star-forming galaxy (DSFG) at z ≈ 5.1. We also present a tentative 2.6σ SCUBA-2 detection at 850 μm around a recently identified z ≈ 16 LBG candidate in the same field and show that, if the emission is real and associated with this candidate, the available photometry is consistent with a z ∼ 5 dusty galaxy with strong nebular emission lines despite its blue near-IR colors. Further observations on this candidate are imperative to mitigate the low confidence of this tentative submillimeter emission and its positional uncertainty. Our analysis shows that robust (sub)millimeter detections of NIRCam dropout galaxies likely imply z ∼ 4–6 redshift solutions, where the observed near-IR break would be the result of a strong rest-frame optical Balmer break combined with high dust attenuation and strong nebular line emission, rather than the rest-frame UV Lyman break. This provides evidence that DSFGs may contaminate searches for ultra-high redshift LBG candidates from JWST observations.

Published
2023

10. A Long Time Ago in a Galaxy Far, Far Away: A Candidate z ~ 12 Galaxy in Early JWST CEERS Imaging

Author

Finkelstein, SL, Bagley, MB, Haro, PA, Dickinson, M, Ferguson, HC, Kartaltepe, JS, Papovich, C, Burgarella, D, Kocevski, DD, Huertas-Company, M, Iyer, KG, Koekemoer, AM, Larson, RL, Pérez-González, PG, Rose, C, Tacchella, S, Wilkins, SM, Chworowsky, K, Medrano, A, Morales, AM, Somerville, RS, Aaron Yung, LY, Fontana, A, Giavalisco, M, Grazian, A, Grogin, NA, Kewley, LJ, Kirkpatrick, A, Kurczynski, P, Lotz, JM, Pentericci, L, Pirzkal, N, Ravindranath, S, Ryan, RE, Trump, Yang, G, Almaini, O, Amorín, RO, Annunziatella, M, Backhaus, BE, Barro, G, Behroozi, P, Bell, EF, Bhatawdekar, R, Bisigello, L, Bromm, V, Buat, V, Buitrago, F, Calabrò, A, Casey, CM, Castellano, M, Chávez Ortiz, ÓA, Ciesla, L, Cleri, NJ, Cohen, SH, Cole, JW, Cooke, KC, Cooper, MC, Cooray, AR, Costantin, L, Cox, IG, Croton, D, Daddi, E, Davé, R, De La Vega, A, Dekel, A, Elbaz, D, Estrada-Carpenter, V, Faber, SM, Fernández, V, Finkelstein, KD, Freundlich, J, Fujimoto, S, García-Argumánez, Á, Gardner, JP, Gawiser, E, Gómez-Guijarro, C, Guo, Y, Hamblin, K, Hamilton, TS, Hathi, NP, Holwerda, BW, Hirschmann, M, Hutchison, TA, Jaskot, AE, Jha, SW, Jogee, S, Juneau, S, Jung, I, Kassin, SA, Le Bail, A, Leung, GCK, Lucas, RA, Magnelli, B, Mantha, KB, Matharu, J, McGrath, EJ, McIntosh, DH, Merlin, E, Mobasher, B, Finkelstein, SL [0000-0001-8519-1130], Bagley, MB [0000-0002-9921-9218], Haro, PA [0000-0002-7959-8783], Dickinson, M [0000-0001-5414-5131], Ferguson, HC [0000-0001-7113-2738], Kartaltepe, JS [0000-0001-9187-3605], Papovich, C [0000-0001-7503-8482], Burgarella, D [0000-0002-4193-2539], Kocevski, DD [0000-0002-8360-3880], Huertas-Company, M [0000-0002-1416-8483], Iyer, KG [0000-0001-9298-3523], Koekemoer, AM [0000-0002-6610-2048], Larson, RL [0000-0003-2366-8858], Pérez-González, PG [0000-0003-4528-5639], Rose, C [0000-0002-8018-3219], Tacchella, S [0000-0002-8224-4505], Wilkins, SM [0000-0003-3903-6935], Chworowsky, K [0000-0003-4922-0613], Morales, AM [0000-0003-4965-0402], Somerville, RS [0000-0002-6748-6821], Aaron Yung, LY [0000-0003-3466-035X], Fontana, A [0000-0003-3820-2823], Giavalisco, M [0000-0002-7831-8751], Grazian, A [0000-0002-5688-0663], Grogin, NA [0000-0001-9440-8872], Kewley, LJ [0000-0001-8152-3943], Kirkpatrick, A [0000-0002-1306-1545], Kurczynski, P [0000-0002-8816-5146], Lotz, JM [0000-0003-3130-5643], Pentericci, L [0000-0001-8940-6768], Pirzkal, N [0000-0003-3382-5941], Ravindranath, S [0000-0002-5269-6527], Ryan, RE [0000-0003-0894-1588], Trump, JR [0000-0002-1410-0470], Yang, G [0000-0001-8835-7722], Almaini, O [0000-0001-9328-3991], Amorín, RO [0000-0001-5758-1000], Annunziatella, M [0000-0002-8053-8040], Backhaus, BE [0000-0001-8534-7502], Behroozi, P [0000-0002-2517-6446], Bell, EF [0000-0002-5564-9873], Bhatawdekar, R [0000-0003-0883-2226], Bisigello, L [0000-0003-0492-4924], Bromm, V [0000-0003-0212-2979], Buat, V [0000-0003-3441-903X], Buitrago, F [0000-0002-2861-9812], Calabrò, A [0000-0003-2536-1614], Casey, CM [0000-0002-0930-6466], Castellano, M [0000-0001-9875-8263], Chávez Ortiz, ÓA [0000-0003-2332-5505], Ciesla, L [0000-0003-0541-2891], Cleri, NJ [0000-0001-7151-009X], Cohen, SH [0000-0003-3329-1337], Cole, JW [0000-0002-6348-1900], Cooke, KC [0000-0002-2200-9845], Cooper, MC [0000-0003-1371-6019], Cooray, AR [0000-0002-3892-0190], Costantin, L [0000-0001-6820-0015], Cox, IG [0000-0002-1803-794X], Croton, D [0000-0002-5009-512X], Daddi, E [0000-0002-3331-9590], Davé, R [0000-0003-2842-9434], De La Vega, A [0000-0002-6219-5558], Dekel, A [0000-0003-4174-0374], Elbaz, D [0000-0002-7631-647X], Estrada-Carpenter, V [0000-0001-8489-2349], Fernández, V [0000-0003-0531-5450], Finkelstein, KD [0000-0003-0792-5877], Freundlich, J [0000-0002-5245-7796], Fujimoto, S [0000-0001-7201-5066], García-Argumánez, Á [0000-0002-8365-5525], Gardner, JP [0000-0003-2098-9568], Gawiser, E [0000-0003-1530-8713], Gómez-Guijarro, C [0000-0002-4085-9165], Guo, Y [0000-0002-4162-6523], Hamblin, K [0000-0002-6292-4589], Hamilton, TS [0000-0002-9753-1769], Hathi, NP [0000-0001-6145-5090], Holwerda, BW [0000-0002-4884-6756], Hirschmann, M [0000-0002-3301-3321], Hutchison, TA [0000-0001-6251-4988], Jaskot, AE [0000-0002-6790-5125], Jha, SW [0000-0001-8738-6011], Jogee, S [0000-0002-1590-0568], Juneau, S [0000-0002-0000-2394], Jung, I [0000-0003-1187-4240], Kassin, SA [0000-0002-3838-8093], Le Bail, A [0000-0002-9466-2763], Leung, GCK [0000-0002-9393-6507], Lucas, RA [0000-0003-1581-7825], Magnelli, B [0000-0002-6777-6490], Matharu, J [0000-0002-7547-3385], McGrath, EJ [0000-0001-8688-2443], Merlin, E [0000-0001-6870-8900], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, 5109 Space Sciences, 51 Physical Sciences, Galaxies and Cosmology
Abstract

We report the discovery of a candidate galaxy with a photo-z of z ∼ 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 z phot = 11.8 − 0.2 + 0.3 (1σ uncertainty) with m F200W = 27.3 and ≳7σ detections in five filters. The source is not detected at λ < 1.4 μm in deep imaging from both Hubble Space Telescope (HST) and JWST and has faint ∼3σ detections in JWST F150W and HST F160W, which signal a Lyα break near the red edge of both filters, implying z ∼ 12. This object (Maisie’s Galaxy) exhibits F115W − F200W > 1.9 mag (2σ 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 ⊙ ∼ 8.5 and is highly star-forming (log sSFR ∼ −8.2 yr−1), with a blue rest-UV color (β ∼ −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.

Published
2022
Full Text
View/download PDF

11. The size and pervasiveness of Ly α–UV spatial offsets in star-forming galaxies at z ∼ 6

Author

Lemaux, BC, Fuller, S, Bradač, M, Pentericci, L, Hoag, A, Strait, V, Treu, T, Alvarez, C, Bolan, P, Gandhi, PJ, Huang, K-H, Jones, T, Mason, C, Pelliccia, D, Ribeiro, B, Ryan, RE, Schmidt, KB, Vanzella, E, Khusanova, Y, Le Fèvre, O, Guaita, L, Hathi, NP, Koekemoer, A, and Pforr, J

Subjects
photometric [techniques], strong [gravitational lensing], astro-ph.GA, reionization, spectroscopic [techniques], Astronomy & Astrophysics, evolution [galaxies], high-redshift [galaxies], Astronomical and Space Sciences
Abstract

We study the projected spatial offset between the ultraviolet continuum and Ly α emission for 65 lensed and unlensed galaxies in the Epoch of Reionization (5 ≤ z ≤ 7), the first such study at these redshifts, in order to understand the potential for these offsets to confuse estimates of the Ly α properties of galaxies observed in slit spectroscopy. While we find that ∼40 per cent of galaxies in our sample show significant projected spatial offsets ($|\Delta {\rm {Ly}\alpha -\rm {UV}}|$), we find a relatively modest average projected offset of $|\widetilde{\Delta }{\rm {Ly}\alpha -\rm {UV}}|$ = 0.61 ± 0.08 proper kpc for the entire sample. A small fraction of our sample, ∼10 per cent, exhibit offsets in excess of 2 proper kpc, with offsets seen up to ∼4 proper kpc, sizes that are considerably larger than the effective radii of typical galaxies at these redshifts. An internal comparison and a comparison to studies at lower redshift yielded no significant evidence of evolution of $|\Delta {\rm {Ly}\alpha -\rm {UV}}|$ with redshift. In our sample, ultraviolet (UV)-bright galaxies ($\widetilde{L{\mathrm{ UV}}}/L{\ast }{\mathrm{ UV}}=0.67$) showed offsets a factor of three greater than their fainter counterparts ($\widetilde{L{\mathrm{ UV}}}/L{\ast }{\mathrm{ UV}}=0.10$), 0.89 ± 0.18 versus 0.27 ± 0.05 proper kpc, respectively. The presence of companion galaxies and early stage merging activity appeared to be unlikely causes of these offsets. Rather, these offsets appear consistent with a scenario in which internal anisotropic processes resulting from stellar feedback, which is stronger in UV-brighter galaxies, facilitate Ly α fluorescence and/or backscattering from nearby or outflowing gas. The reduction in the Ly α flux due to offsets was quantified. It was found that the differential loss of Ly α photons for galaxies with average offsets is not, if corrected for, a limiting factor for all but the narrowest slit widths (

Published
2021

12. The ALPINE-ALMA [CII] survey: Survey strategy, observations, and sample properties of 118 star-forming galaxies at 4 < z < 6

Author

Le Fèvre, O, Béthermin, M, Faisst, A, Jones, GC, Capak, P, Cassata, P, Silverman, JD, Schaerer, D, Yan, L, Amorin, R, Bardelli, S, Boquien, M, Cimatti, A, Dessauges-Zavadsky, M, Giavalisco, M, Hathi, NP, Fudamoto, Y, Fujimoto, S, Ginolfi, M, Gruppioni, C, Hemmati, S, Ibar, E, Koekemoer, A, Khusanova, Y, Lagache, G, Lemaux, BC, Loiacono, F, Maiolino, R, Mancini, C, Narayanan, D, Morselli, L, Méndez-Hernàndez, H, Oesch, PA, Pozzi, F, Romano, M, Riechers, D, Scoville, N, Talia, M, Tasca, LAM, Thomas, R, Toft, S, Vallini, L, Vergani, D, Walter, F, Zamorani, G, Zucca, E, Jones, Gareth [0000-0002-0267-9024], Maiolino, Roberto [0000-0002-4985-3819], and Apollo - University of Cambridge Repository

Subjects
galaxies: star formation, galaxies: formation, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

The ALMA-ALPINE [CII] survey is aimed at characterizing the properties of a sample of normal star-forming galaxies (SFGs). The ALMA Large Program to INvestigate (ALPINE) features 118 galaxies observed in the [CII]-158 μm line and far infrared (FIR) continuum emission during the period of rapid mass assembly, right after the end of the HI reionization, at redshifts of 4 < z < 6. We present the survey science goals, the observational strategy, and the sample selection of the 118 galaxies observed with ALMA, with an average beam minor axis of about 0.85″, or ∼5 kpc at the median redshift of the survey. The properties of the sample are described, including spectroscopic redshifts derived from the UV-rest frame, stellar masses, and star-formation rates obtained from a spectral energy distribution (SED) fitting. The observed properties derived from the ALMA data are presented and discussed in terms of the overall detection rate in [CII] and FIR continuum, with the observed signal-to-noise distribution. The sample is representative of the SFG population in the main sequence at these redshifts. The overall detection rate in [CII] is 64% for a signal-to-noise ratio (S/N) threshold larger than 3.5 corresponding to a 95% purity (40% detection rate for S/N > 5). Based on a visual inspection of the [CII] data cubes together with the large wealth of ancillary data, we find a surprisingly wide range of galaxy types, including 40% that are mergers, 20% extended and dispersion-dominated, 13% compact, and 11% rotating discs, with the remaining 16% too faint to be classified. This diversity indicates that a wide array of physical processes must be at work at this epoch, first and foremost, those of galaxy mergers. This paper sets a reference sample for the gas distribution in normal SFGs at 4 < z < 6, a key epoch in galaxy assembly, which is ideally suited for studies with future facilities, such as the James Webb Space Telescope (JWST) and the Extremely Large Telescopes (ELTs).

Published
2021
Full Text
View/download PDF

13. The ALPINE-ALMA [CII] Survey: CGM pollution and gas mixing by tidal stripping in a merging system at z~4.57

Author

Ginolfi, M, Jones, GC, Bethermin, M, Faisst, A, Lemaux, BC, Schaerer, D, Fudamoto, Y, Oesch, P, Dessauges-Zavadsky, M, Fujimoto, S, Carniani, S, Fevre, O Le, Cassata, P, Silverman, JD, Capak, P, Yan, Lin, Bardelli, S, Cucciati, O, Gal, R, Gruppioni, C, Hathi, NP, Lubin, L, Maiolino, R, Morselli, L, Pelliccia, D, Talia, M, Vergani, D, Zamorani, G, Jones, Gareth [0000-0002-0267-9024], Maiolino, Roberto [0000-0002-4985-3819], and Apollo - University of Cambridge Repository

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present ALMA observations of a merging system at z ~ 4.57, observed as a part of the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) survey. Combining ALMA [CII] 158 micron and far-infrared continuum data with multi-wavelength ancillary data we find that the system is composed of two massive (Mstar >~ 10^10 Msun) star-forming galaxies experiencing a major merger (stellar mass ratio r_mass ~ 0.9) at close spatial (~13 kpc; projected) and velocity (delta_v < 300 km/s) separations, and two additional faint narrow [CII]-emitting satellites. The overall system belongs to a larger-scale protocluster environment and is coincident to one of its overdensity peaks. ALMA reveals also the presence of [CII] emission arising from a circumgalactic gas structure, extending up to a diameter-scale of ~30 kpc. Our morpho-spectral decomposition analysis shows that about 50% of the total flux resides between the individual galaxy components, in a metal-enriched gaseous envelope characterized by a disturbed morphology and complex kinematics. Similarly to observations of shock-excited [CII] emitted from tidal tails in local groups, our results can be interpreted as a possible signature of interstellar gas stripped by strong gravitational interactions, with a possible contribution from material ejected by galactic outflows and emission triggered by star formation in small faint satellites. Our findings suggest that mergers could be an efficient mechanism of gas mixing in the circumgalactic medium around high-z galaxies, and thus play a key role in the galaxy baryon cycle at early epochs., 12 pages, 7 figures. Accepted for publication in A&A

Published
2020
Full Text
View/download PDF

14. The VIMOS Ultra Deep Survey: The role of HI kinematics and HI column density on the escape of Lyα photons in star-forming galaxies at 2 < z < 4

Author

Guaita, L, Talia, M, Pentericci, L, Verhamme, A, Cassata, P, Lemaux, BC, Orlitova, I, Ribeiro, B, Schaerer, D, Zamorani, G, Garilli, B, Le Brun, V, Le Fèvre, O, MacCagni, D, Tasca, LAM, Thomas, R, Vanzella, E, Zucca, E, Amorin, R, Bardelli, S, Castellano, M, Grazian, A, Hathi, NP, Koekemoer, A, and Marchi, F

Subjects
ISM: kinematics and dynamics, techniques: imaging spectroscopy, galaxies: high-redshift, galaxies: star formation, scattering
Abstract

© 2017 ESO. Aims. We wish to assess the role of kinematics and neutral hydrogen column density in the escape and distribution of Lya photons. Methods. We selected a sample of 76 Lya emitting galaxies from the VIMOS Ultra Deep Survey (VUDS) at 2 = z = 4. We estimated the velocity of the neutral gas flowing out of the interstellar medium as the velocity offset, δv, between the systemic redshift (zsys) and the center of low-ionization absorption line systems (LIS). To increase the S/N of VUDS spectra, we stacked subsamples defined based on median values of their photometric and spectroscopic properties. We measured the systemic redshift from the rest-frame UV spectroscopic data using the CIII]1908 nebular emission line, and we considered SiII1526 as the highest signal-to-noise LIS line. We calculated the Lya peak shift with respect to the zsys, the EW(Lya), and the Lya spatial extension, Ext(Lya-C), from the in the 2D stacked spectra. Results. The galaxies that are faint in the rest-frame UV continuum, strong in Lya and CIII] , with compact UV morphology, and localized in an underdense environment are characterized by outflow velocities of the order of a few hundreds of km s -1 . The subsamples with smaller δv are characterized by larger Lya peak shifts, larger Ext(Lya-C), and smaller EW(Lya). In general we find that EW(Lya) anti-correlates with Ext(Lya-C) and Lya peak shift. Conclusions. We interpret these trends using a radiative-transfer shell model. The model predicts that an HI gas with a column density larger than 1020 cm -2 is able to produce Lya peak shifts larger than > 300 km s -1 . An ISM with this value of NHI would favour a large amount of scattering events, especially when the medium is static, so it can explain large values of Ext(Lya-C) and small EW(Lya). On the contrary, an ISM with a lower NHI, but large velocity outflows would lead to a Lya spatial profile peaked at the galaxy center (i.e. low values of Ext(Lya-C)) and to a large EW(Lya), as we see in our data. Our results and their interpretation via radiative-transfer models tell us that it is possible to use Lya to study the properties of the HI gas. Also, the fact that Lya emitters are characterized by large δv could give hints about their stage of evolution in the sense that they could be experiencing short bursts of star formation that push strong outflows., This work is supported by funding from the European Research Council Advanced Grant ERC–2010–AdG–268107–EARLY and by INAF Grants PRIN 2010, PRIN 2012, and PICS 2013. This work is based on data products made available at the CESAM data center, Laboratoire d’Astrophysique de Marseille, France. R.A. acknowledges support from the ERC Advanced Grant 695671 “QUENCH” and I.O. from the Czech Science Foundation grant 17-06217Y.

Published
2017
Full Text
View/download PDF

15. AGN-enhanced outflows of low-ionization gas in star-forming galaxies at 1.7 < z < 4.6

Author

Talia, M, Brusa, M, Cimatti, A, Lemaux, BC, Amorin, R, Bardelli, S, Cassarà, LP, Cucciati, O, Garilli, B, Grazian, A, Guaita, L, Hathi, NP, Koekemoer, A, Fèvre, OL, Maccagni, D, Nakajima, K, Pentericci, L, Pforr, J, Schaerer, D, Vanzella, E, Vergani, D, Zamorani, G, and Zucca, E

Subjects
ISM: jets and outflows, galaxies: high-redshift, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, ultraviolet: ISM, Astrophysics::Galaxy Astrophysics, galaxies: ISM
Abstract

Fast and energetic winds are invoked by galaxy formation models as essential processes in the evolution of galaxies. These outflows can be powered either by star formation (SF) and/or active galactic nucleus (AGN) activity, but the relative dominance of the two mechanisms is still under debate. We use spectroscopic stacking analysis to study the properties of the low-ionization phase of the outflow in a sample of 1330 star-forming galaxies (SFGs) and 79 X-ray-detected (1042 < LX < 1045 erg s−1) Type 2 AGN at 1.7 < z < 4.6 selected from a compilation of deep optical spectroscopic surveys, mostly zCOSMOS-Deep and VIMOS Ultra Deep Survey (VUDS). We measure mean velocity offsets of ∼− 150 km s−1 in the SFGs, while in the AGN sample the velocity is much higher (∼− 950 km s−1), suggesting that the AGN is boosting the outflow up to velocities that could not be reached only with the SF contribution. The sample of X-ray AGN has on average a lower SF rate than non-AGN SFGs of similar mass: this, combined with the enhanced outflow velocity in AGN hosts, is consistent with AGN feedback in action. We further divide our sample of AGN into two X-ray luminosity bins: we measure the same velocity offsets in both stacked spectra, at odds with results reported for the highly ionized phase in local AGN, suggesting that the two phases of the outflow may be mixed only up to relatively low velocities, while the highest velocities can be reached only by the highly ionized phase., This work is supported by funding from the European Research Council Advanced Grant ERC–2010–AdG–268107–EARLY and by INAF Grants PRIN 2010, PRIN 2012 and PICS 2013. AC, OC, and MT acknowledge the grant MIUR PRIN 2010–2011. MB acknowledges support from the FP7 grant ‘eEASy’: (CIG 321913). RA acknowledges support from the ERC Advanced Grant 695671 ‘QUENCH’. We acknowledge the grants ASI n.I/023/12/0 ‘Attività relative alla fase B2/C per la missione Euclid’ and MIUR PRIN 2010-2011 ‘The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid’ and PRIN MIUR 2015 ‘Cosmology and Fundamental Physics: illuminating the Dark Universe with Euclid’.

Published
2017
Full Text
View/download PDF

16. The VIMOS Ultra-Deep Survey: A major merger origin for the high fraction of galaxies at 2 < z < 6 with two bright clumps

Author

Ribeiro, B, Le Fèvre, O, Cassata, P, Garilli, B, Lemaux, BC, Maccagni, D, Schaerer, D, Tasca, LAM, Zamorani, G, Zucca, E, Amorín, R, Bardelli, S, Hathi, NP, Koekemoer, A, Pforr, J, Amorin Barbieri, Ricardo [0000-0001-5758-1000], and Apollo - University of Cambridge Repository

Subjects
galaxies: high-redshift, Astrophysics::Solar and Stellar Astrophysics, galaxies: structure, galaxies: formation, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

(Abridged) The properties of stellar clumps in star forming galaxies and their evolution over the redshift range $2\lesssim z \lesssim 6$ are presented and discussed in the context of the build-up of massive galaxies at early cosmic times. We use HST/ACS images of galaxies with spectroscopic redshifts from the VIMOS Ultra Deep Survey (VUDS) to identify clumps within a 20 kpc radius. We find that the population of galaxies with more than one clump is dominated by galaxies with two clumps, representing $\sim21-25$\% of the population, while the fraction of galaxies with 3, or 4 and more, clumps is 8-11 and 7-9\%, respectively. The fraction of clumpy galaxies is in the range $\sim35-55\%$ over $2

Published
2017

17. Candels: The cosmic assembly near-infrared deep extragalactic legacy survey - The hubble space telescope observations, imaging data products, and mosaics

Author

Koekemoer, A, Faber, S, Ferguson, H, Grogin, N, Kocevski, D, Koo, D, Lai, K, Lotz, J, Lucas, R, Mcgrath, E, Ogaz, S, Rajan, A, Riess, A, Rodney, S, Strolger, L, Casertano, S, Castellano, M, Dahlen, T, Dickinson, M, Dolch, T, Fontana, A, Giavalisco, M, Grazian, A, Guo, Y, Hathi, N, Huang, K, van der Wel, A, Yan, H, Acquaviva, V, Alexander, D, Almaini, O, Ashby, M, Barden, M, Bell, E, Bournaud, F, Brown, T, Caputi, K, Cassata, P, Challis, P, Chary, R, Cheung, E, Cirasuolo, M, Conselice, C, Cooray, A, Croton, D, Daddi, E, Davé, R, de Mello, D, de Ravel, L, Dekel, A, Donley, J, Dunlop, J, Dutton, A, Elbaz, D, Fazio, G, Filippenko, A, Finkelstein, S, Frazer, C, Gardner, J, Garnavich, P, Gawiser, E, Gruetzbauch, R, Hartley, W, Häussler, B, Herrington, J, Hopkins, P, Huang, J, Jha, S, Johnson, A, Kartaltepe, J, Khostovan, A, Kirshner, R, Lani, C, Lee, K, Li, W, Madau, P, Mccarthy, P, Mcintosh, D, Mclure, R, Mcpartland, C, Mobasher, B, Moreira, H, Mortlock, A, Moustakas, L, Mozena, M, Nandra, K, Newman, J, Nielsen, J, Niemi, S, Noeske, K, Papovich, C, Pentericci, L, Pope, A, Primack, J, Ravindranath, S, Reddy, N, Renzini, A, Rix, H, Robaina, A, Rosario, D, Rosati, P, Salimbeni, S, Scarlata, C, Siana, B, Simard, L, Smidt, J, Snyder, D, Somerville, R, Spinrad, H, Straughn, A, Telford, O, Teplitz, H, Trump, J, Vargas, C, Villforth, C, Wagner, C, Wandro, P, Wechsler, R, Weiner, B, Wiklind, T, Wild, V, Wilson, G, Wuyts, S, Yun, M, Koekemoer, AM, Faber, SM, Ferguson, HC, Grogin, NA, Kocevski, DD, Koo, DC, Lotz, JM, Lucas, RA, McGrath, EJ, Riess, AG, Rodney, SA, Guo, YC, Hathi, NP, Huang, KH, Yan, HJ, Alexander, DM, Ashby, MLN, Bell, EF, Brown, TM, Caputi, KI, Challis, PJ, Chary, RR, Conselice, CJ, Cooray, AR, Croton, DJ, de Mello, DF, Donley, JL, Dunlop, JS, Dutton, AA, Fazio, GG, Filippenko, AV, Finkelstein, SL, Gardner, JP, Garnavich, PM, Hartley, WG, Hopkins, PF, Huang, JS, Jha, SW, Kartaltepe, JS, Khostovan, AA, Kirshner, RP, Lee, KS, Li, WD, McCarthy, PJ, McIntosh, DH, McLure, RJ, McPartland, C, Moustakas, LA, Newman, JA, Nielsen, JL, Noeske, KG, Papovich, CJ, Primack, JR, Reddy, NA, Rix, HW, Robaina, AR, Rosario, DJ, Somerville, RS, Straughn, AN, Teplitz, HI, Trump, JR, Wagner, CR, Wechsler, RH, Weiner, BJ, Yun, MS, Koekemoer, A, Faber, S, Ferguson, H, Grogin, N, Kocevski, D, Koo, D, Lai, K, Lotz, J, Lucas, R, Mcgrath, E, Ogaz, S, Rajan, A, Riess, A, Rodney, S, Strolger, L, Casertano, S, Castellano, M, Dahlen, T, Dickinson, M, Dolch, T, Fontana, A, Giavalisco, M, Grazian, A, Guo, Y, Hathi, N, Huang, K, van der Wel, A, Yan, H, Acquaviva, V, Alexander, D, Almaini, O, Ashby, M, Barden, M, Bell, E, Bournaud, F, Brown, T, Caputi, K, Cassata, P, Challis, P, Chary, R, Cheung, E, Cirasuolo, M, Conselice, C, Cooray, A, Croton, D, Daddi, E, Davé, R, de Mello, D, de Ravel, L, Dekel, A, Donley, J, Dunlop, J, Dutton, A, Elbaz, D, Fazio, G, Filippenko, A, Finkelstein, S, Frazer, C, Gardner, J, Garnavich, P, Gawiser, E, Gruetzbauch, R, Hartley, W, Häussler, B, Herrington, J, Hopkins, P, Huang, J, Jha, S, Johnson, A, Kartaltepe, J, Khostovan, A, Kirshner, R, Lani, C, Lee, K, Li, W, Madau, P, Mccarthy, P, Mcintosh, D, Mclure, R, Mcpartland, C, Mobasher, B, Moreira, H, Mortlock, A, Moustakas, L, Mozena, M, Nandra, K, Newman, J, Nielsen, J, Niemi, S, Noeske, K, Papovich, C, Pentericci, L, Pope, A, Primack, J, Ravindranath, S, Reddy, N, Renzini, A, Rix, H, Robaina, A, Rosario, D, Rosati, P, Salimbeni, S, Scarlata, C, Siana, B, Simard, L, Smidt, J, Snyder, D, Somerville, R, Spinrad, H, Straughn, A, Telford, O, Teplitz, H, Trump, J, Vargas, C, Villforth, C, Wagner, C, Wandro, P, Wechsler, R, Weiner, B, Wiklind, T, Wild, V, Wilson, G, Wuyts, S, Yun, M, Koekemoer, AM, Faber, SM, Ferguson, HC, Grogin, NA, Kocevski, DD, Koo, DC, Lotz, JM, Lucas, RA, McGrath, EJ, Riess, AG, Rodney, SA, Guo, YC, Hathi, NP, Huang, KH, Yan, HJ, Alexander, DM, Ashby, MLN, Bell, EF, Brown, TM, Caputi, KI, Challis, PJ, Chary, RR, Conselice, CJ, Cooray, AR, Croton, DJ, de Mello, DF, Donley, JL, Dunlop, JS, Dutton, AA, Fazio, GG, Filippenko, AV, Finkelstein, SL, Gardner, JP, Garnavich, PM, Hartley, WG, Hopkins, PF, Huang, JS, Jha, SW, Kartaltepe, JS, Khostovan, AA, Kirshner, RP, Lee, KS, Li, WD, McCarthy, PJ, McIntosh, DH, McLure, RJ, McPartland, C, Moustakas, LA, Newman, JA, Nielsen, JL, Noeske, KG, Papovich, CJ, Primack, JR, Reddy, NA, Rix, HW, Robaina, AR, Rosario, DJ, Somerville, RS, Straughn, AN, Teplitz, HI, Trump, JR, Wagner, CR, Wechsler, RH, Weiner, BJ, and Yun, MS

Abstract

This paper describes the Hubble Space Telescope imaging data products and data reduction procedures for the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). This survey is designed to document the evolution of galaxies and black holes at z ≈ 1.5-8, and to study Type Ia supernovae at z > 1.5. Five premier multi-wavelength sky regions are selected, each with extensive multi-wavelength observations. The primary CANDELS data consist of imaging obtained in the Wide Field Camera 3 infrared channel (WFC3/IR) and the WFC3 ultraviolet/optical channel, along with the Advanced Camera for Surveys (ACS). The CANDELS/Deep survey covers ∼ 125 arcmin 2 within GOODS-N and GOODS-S, while the remainder consists of the CANDELS/Wide survey, achieving a total of ∼ 800 arcmin2 across GOODS and three additional fields (Extended Groth Strip, COSMOS, and Ultra-Deep Survey). We summarize the observational aspects of the survey as motivated by the scientific goals and present a detailed description of the data reduction procedures and products from the survey. Our data reduction methods utilize the most up-to-date calibration files and image combination procedures. We have paid special attention to correcting a range of instrumental effects, including charge transfer efficiency degradation for ACS, removal of electronic bias-striping present in ACS data after Servicing Mission 4, and persistence effects and other artifacts in WFC3/IR. For each field, we release mosaics for individual epochs and eventual mosaics containing data from all epochs combined, to facilitate photometric variability studies and the deepest possible photometry. A more detailed overview of the science goals and observational design of the survey are presented in a companion paper.

Published
2011

18. The ALPINE-ALMA [CII] Survey: CGM pollution and gas mixing by tidal stripping in a merging system at z~4.57

Author

Ginolfi, M, Jones, GC, Bethermin, M, Faisst, A, Lemaux, BC, Schaerer, D, Fudamoto, Y, Oesch, P, Dessauges-Zavadsky, M, Fujimoto, S, Carniani, S, Fevre, O Le, Cassata, P, Silverman, JD, Capak, P, Yan, Lin, Bardelli, S, Cucciati, O, Gal, R, Gruppioni, C, Hathi, NP, Lubin, L, Maiolino, R, Morselli, L, Pelliccia, D, Talia, M, Vergani, D, and Zamorani, G

Subjects
13. Climate action, astro-ph.GA, astro-ph.CO, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, 6. Clean water
Abstract

We present ALMA observations of a merging system at z ~ 4.57, observed as a part of the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) survey. Combining ALMA [CII] 158 micron and far-infrared continuum data with multi-wavelength ancillary data we find that the system is composed of two massive (Mstar >~ 10^10 Msun) star-forming galaxies experiencing a major merger (stellar mass ratio r_mass ~ 0.9) at close spatial (~13 kpc; projected) and velocity (delta_v < 300 km/s) separations, and two additional faint narrow [CII]-emitting satellites. The overall system belongs to a larger-scale protocluster environment and is coincident to one of its overdensity peaks. ALMA reveals also the presence of [CII] emission arising from a circumgalactic gas structure, extending out to ~30 kpc. Our morpho-spectral decomposition analysis shows that about 50% of the total flux resides between the individual galaxy components, in a metal-enriched gaseous envelope characterized by a disturbed morphology and complex kinematics. Similarly to observations of shock-excited [CII] emitted from tidal tails in local groups, our results can be interpreted as a possible signature of interstellar gas stripped by strong gravitational interactions, with a possible contribution from material ejected by galactic outflows and emission triggered by star formation in small faint satellites. Our findings suggest that mergers could be an efficient mechanism of gas mixing in the circumgalactic medium around high-z galaxies, and thus play a key role in the galaxy baryon cycle at early epochs., STFC, ERC

19. CEERS Key Paper. II. A First Look at the Resolved Host Properties of AGN at 3 < z < 5 with JWST

Author

Dale D. Kocevski, Guillermo Barro, Elizabeth J. McGrath, Steven L. Finkelstein, Micaela B. Bagley, Henry C. Ferguson, Shardha Jogee, Guang Yang, Mark Dickinson, Nimish P. Hathi, Bren E. Backhaus, Eric F. Bell, Laura Bisigello, Véronique Buat, Denis Burgarella, Caitlin M. Casey, Nikko J. Cleri, M. C. Cooper, Luca Costantin, Darren Croton, Emanuele Daddi, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Eric Gawiser, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Pablo Arrabal Haro, Michaela Hirschmann, Benne W. Holwerda, Marc Huertas-Company, Taylor A. Hutchison, Kartheik G. Iyer, Brenda Jones, Stéphanie Juneau, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, Peter Kurczynski, Aurélien Le Bail, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Rachel S. Somerville, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Stephen M. Wilkins, Stijn Wuyts, L. Y. Aaron Yung, Jorge A. Zavala, Kocevski, DD [0000-0002-8360-3880], Barro, G [0000-0002-0786-7307], McGrath, EJ [0000-0001-8688-2443], Finkelstein, SL [0000-0001-8519-1130], Bagley, MB [0000-0002-9921-9218], Ferguson, HC [0000-0001-7113-2738], Jogee, S [0000-0002-1590-0568], Yang, G [0000-0001-8835-7722], Dickinson, M [0000-0001-5414-5131], Hathi, NP [0000-0001-6145-5090], Backhaus, BE [0000-0001-8534-7502], Bell, EF [0000-0002-5564-9873], Bisigello, L [0000-0003-0492-4924], Buat, V [0000-0003-3441-903X], Burgarella, D [0000-0002-4193-2539], Casey, CM [0000-0002-0930-6466], Cleri, NJ [0000-0001-7151-009X], Cooper, MC [0000-0003-1371-6019], Costantin, L [0000-0001-6820-0015], Croton, D [0000-0002-5009-512X], Daddi, E [0000-0002-3331-9590], Fontana, A [0000-0003-3820-2823], Fujimoto, S [0000-0001-7201-5066], Gardner, JP [0000-0003-2098-9568], Gawiser, E [0000-0003-1530-8713], Giavalisco, M [0000-0002-7831-8751], Grazian, A [0000-0002-5688-0663], Grogin, NA [0000-0001-9440-8872], Guo, Y [0000-0002-4162-6523], Haro, PA [0000-0002-7959-8783], Hirschmann, M [0000-0002-3301-3321], Holwerda, BW [0000-0002-4884-6756], Huertas-Company, M [0000-0002-1416-8483], Hutchison, TA [0000-0001-6251-4988], Iyer, KG [0000-0001-9298-3523], Juneau, S [0000-0002-0000-2394], Kartaltepe, JS [0000-0001-9187-3605], Kewley, LJ [0000-0001-8152-3943], Kirkpatrick, A [0000-0002-1306-1545], Koekemoer, AM [0000-0002-6610-2048], Kurczynski, P [0000-0002-8816-5146], Bail, AL [0000-0002-9466-2763], Long, AS [0000-0002-7530-8857], Lotz, JM [0000-0003-3130-5643], Lucas, RA [0000-0003-1581-7825], Papovich, C [0000-0001-7503-8482], Pentericci, L [0000-0001-8940-6768], Pérez-González, PG [0000-0003-4528-5639], Pirzkal, N [0000-0003-3382-5941], Rafelski, M [0000-0002-9946-4731], Ravindranath, S [0000-0002-5269-6527], Somerville, RS [0000-0002-6748-6821], Straughn, AN [0000-0002-4772-7878], Tacchella, S [0000-0002-8224-4505], Trump, JR [0000-0002-1410-0470], Wilkins, SM [0000-0003-3903-6935], Wuyts, S [0000-0003-3735-1931], Aaron Yung, LY [0000-0003-3466-035X], Zavala, JA [0000-0002-7051-1100], Apollo - University of Cambridge Repository, Kocevski, Dale D [0000-0002-8360-3880], Barro, Guillermo [0000-0002-0786-7307], McGrath, Elizabeth J [0000-0001-8688-2443], Finkelstein, Steven L [0000-0001-8519-1130], Bagley, Micaela B [0000-0002-9921-9218], Ferguson, Henry C [0000-0001-7113-2738], Jogee, Shardha [0000-0002-1590-0568], Yang, Guang [0000-0001-8835-7722], Dickinson, Mark [0000-0001-5414-5131], Hathi, Nimish P [0000-0001-6145-5090], Backhaus, Bren E [0000-0001-8534-7502], Bell, Eric F [0000-0002-5564-9873], Bisigello, Laura [0000-0003-0492-4924], Buat, Véronique [0000-0003-3441-903X], Burgarella, Denis [0000-0002-4193-2539], Casey, Caitlin M [0000-0002-0930-6466], Cleri, Nikko J [0000-0001-7151-009X], Costantin, Luca [0000-0001-6820-0015], Croton, Darren [0000-0002-5009-512X], Daddi, Emanuele [0000-0002-3331-9590], Fontana, Adriano [0000-0003-3820-2823], Fujimoto, Seiji [0000-0001-7201-5066], Gardner, Jonathan P [0000-0003-2098-9568], Gawiser, Eric [0000-0003-1530-8713], Giavalisco, Mauro [0000-0002-7831-8751], Grazian, Andrea [0000-0002-5688-0663], Grogin, Norman A [0000-0001-9440-8872], Guo, Yuchen [0000-0002-4162-6523], Haro, Pablo Arrabal [0000-0002-7959-8783], Hirschmann, Michaela [0000-0002-3301-3321], Holwerda, Benne W [0000-0002-4884-6756], Huertas-Company, Marc [0000-0002-1416-8483], Hutchison, Taylor A [0000-0001-6251-4988], Iyer, Kartheik G [0000-0001-9298-3523], Juneau, Stéphanie [0000-0002-0000-2394], Kartaltepe, Jeyhan S [0000-0001-9187-3605], Kewley, Lisa J [0000-0001-8152-3943], Kirkpatrick, Allison [0000-0002-1306-1545], Koekemoer, Anton M [0000-0002-6610-2048], Kurczynski, Peter [0000-0002-8816-5146], Bail, Aurélien Le [0000-0002-9466-2763], Long, Arianna S [0000-0002-7530-8857], Lotz, Jennifer M [0000-0003-3130-5643], Lucas, Ray A [0000-0003-1581-7825], Papovich, Casey [0000-0001-7503-8482], Pentericci, Laura [0000-0001-8940-6768], Pérez-González, Pablo G [0000-0003-4528-5639], Pirzkal, Nor [0000-0003-3382-5941], Rafelski, Marc [0000-0002-9946-4731], Ravindranath, Swara [0000-0002-5269-6527], Somerville, Rachel S [0000-0002-6748-6821], Straughn, Amber N [0000-0002-4772-7878], Tacchella, Sandro [0000-0002-8224-4505], Trump, Jonathan R [0000-0002-1410-0470], Wilkins, Stephen M [0000-0003-3903-6935], Wuyts, Stijn [0000-0003-3735-1931], and Zavala, Jorge A [0000-0002-7051-1100]

Subjects
Space and Planetary Science, 5101 Astronomical Sciences, Astronomy and Astrophysics, 51 Physical Sciences, Galaxies and Cosmology
Abstract

We report on the host properties of five X-ray-luminous active galactic nuclei (AGN) identified at 3 < z < 5 in the first epoch of imaging from the Cosmic Evolution Early Release Science Survey. Each galaxy has been imaged with the JWST Near-Infrared Camera, which provides rest-frame optical morphologies at these redshifts. We also derive stellar masses and star formation rates for each host by fitting its spectral energy distribution using a combination of galaxy and AGN templates. We find that three of the AGN hosts have spheroidal morphologies, one is a bulge-dominated disk, and one is dominated by pointlike emission. None are found to show strong morphological disturbances that might indicate a recent interaction or merger event. When compared to a sample of mass-matched inactive galaxies, we find that the AGN hosts have morphologies that are less disturbed and more bulge-dominated. Notably, all four of the resolved hosts have rest-frame optical colors consistent with a quenched or poststarburst stellar population. The presence of AGN in passively evolving galaxies at z > 3 is significant because a rapid feedback mechanism is required in most semianalytic models and cosmological simulations to explain the growing population of massive quiescent galaxies observed at these redshifts. Our findings show that AGN can continue to inject energy into these systems after their star formation is curtailed, potentially heating their halos and preventing renewed star formation. Additional observations will be needed to determine what role this feedback may play in helping to quench these systems and/or maintain their quiescent state.

Published
2023
Full Text
View/download PDF

20. The Physical Conditions of Emission-line Galaxies at Cosmic Dawn from JWST/NIRSpec Spectroscopy in the SMACS 0723 Early Release Observations

Author

Jonathan R. Trump, Pablo Arrabal Haro, Raymond C. Simons, Bren E. Backhaus, Ricardo O. Amorín, Mark Dickinson, Vital Fernández, Casey Papovich, David C. Nicholls, Lisa J. Kewley, Samantha W. Brunker, John J. Salzer, Stephen M. Wilkins, Omar Almaini, Micaela B. Bagley, Danielle A. Berg, Rachana Bhatawdekar, Laura Bisigello, Véronique Buat, Denis Burgarella, Antonello Calabrò, Caitlin M. Casey, Laure Ciesla, Nikko J. Cleri, Justin W. Cole, M. C. Cooper, Asantha R. Cooray, Luca Costantin, Darren Croton, Henry C. Ferguson, Steven L. Finkelstein, Seiji Fujimoto, Jonathan P. Gardner, Eric Gawiser, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Marc Huertas-Company, Taylor A. Hutchison, Shardha Jogee, Stéphanie Juneau, Intae Jung, Jeyhan S. Kartaltepe, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Jennifer M. Lotz, Ray A. Lucas, Benjamin Magnelli, Jasleen Matharu, Pablo G. Pérez-González, Nor Pirzkal, Marc Rafelski, Caitlin Rose, Lise-Marie Seillé, Rachel S. Somerville, Amber N. Straughn, Sandro Tacchella, Brittany N. Vanderhoof, Benjamin J. Weiner, Stijn Wuyts, L. Y. Aaron Yung, Jorge A. Zavala, Trump, Jonathan R [0000-0002-1410-0470], Haro, Pablo Arrabal [0000-0002-7959-8783], Simons, Raymond C [0000-0002-6386-7299], Backhaus, Bren E [0000-0001-8534-7502], Amorín, Ricardo O [0000-0001-5758-1000], Dickinson, Mark [0000-0001-5414-5131], Fernández, Vital [0000-0003-0531-5450], Papovich, Casey [0000-0001-7503-8482], Nicholls, David C [0000-0003-0892-5203], Kewley, Lisa J [0000-0001-8152-3943], Brunker, Samantha W [0000-0001-6776-2550], Salzer, John J [0000-0001-8483-603X], Wilkins, Stephen M [0000-0003-3903-6935], Almaini, Omar [0000-0001-9328-3991], Bagley, Micaela B [0000-0002-9921-9218], Berg, Danielle A [0000-0002-4153-053X], Bhatawdekar, Rachana [0000-0003-0883-2226], Bisigello, Laura [0000-0003-0492-4924], Buat, Véronique [0000-0003-3441-903X], Burgarella, Denis [0000-0002-4193-2539], Calabrò, Antonello [0000-0003-2536-1614], Casey, Caitlin M [0000-0002-0930-6466], Ciesla, Laure [0000-0003-0541-2891], Cleri, Nikko J [0000-0001-7151-009X], Cole, Justin W [0000-0002-6348-1900], Cooper, MC [0000-0003-1371-6019], Cooray, Asantha R [0000-0002-3892-0190], Costantin, Luca [0000-0001-6820-0015], Croton, Darren [0000-0002-5009-512X], Ferguson, Henry C [0000-0001-7113-2738], Finkelstein, Steven L [0000-0001-8519-1130], Fujimoto, Seiji [0000-0001-7201-5066], Gardner, Jonathan P [0000-0003-2098-9568], Gawiser, Eric [0000-0003-1530-8713], Giavalisco, Mauro [0000-0002-7831-8751], Grazian, Andrea [0000-0002-5688-0663], Grogin, Norman A [0000-0001-9440-8872], Hathi, Nimish P [0000-0001-6145-5090], Hirschmann, Michaela [0000-0002-3301-3321], Holwerda, Benne W [0000-0002-4884-6756], Huertas-Company, Marc [0000-0002-1416-8483], Hutchison, Taylor A [0000-0001-6251-4988], Jogee, Shardha [0000-0002-1590-0568], Juneau, Stéphanie [0000-0002-0000-2394], Jung, Intae [0000-0003-1187-4240], Kartaltepe, Jeyhan S [0000-0001-9187-3605], Kirkpatrick, Allison [0000-0002-1306-1545], Kocevski, Dale D [0000-0002-8360-3880], Koekemoer, Anton M [0000-0002-6610-2048], Lotz, Jennifer M [0000-0003-3130-5643], Lucas, Ray A [0000-0003-1581-7825], Magnelli, Benjamin [0000-0002-6777-6490], Matharu, Jasleen [0000-0002-7547-3385], Pérez-González, Pablo G [0000-0003-4528-5639], Pirzkal, Nor [0000-0003-3382-5941], Rafelski, Marc [0000-0002-9946-4731], Rose, Caitlin [0000-0002-8018-3219], Seillé, Lise-Marie [0000-0001-7755-4755], Somerville, Rachel S [0000-0002-6748-6821], Straughn, Amber N [0000-0002-4772-7878], Tacchella, Sandro [0000-0002-8224-4505], Vanderhoof, Brittany N [0000-0002-8163-0172], Weiner, Benjamin J [0000-0001-6065-7483], Wuyts, Stijn [0000-0003-3735-1931], Aaron Yung, LY [0000-0003-3466-035X], Zavala, Jorge A [0000-0002-7051-1100], Apollo - University of Cambridge Repository, Trump, JR [0000-0002-1410-0470], Haro, PA [0000-0002-7959-8783], Simons, RC [0000-0002-6386-7299], Backhaus, BE [0000-0001-8534-7502], Amorín, RO [0000-0001-5758-1000], Dickinson, M [0000-0001-5414-5131], Fernández, V [0000-0003-0531-5450], Papovich, C [0000-0001-7503-8482], Nicholls, DC [0000-0003-0892-5203], Kewley, LJ [0000-0001-8152-3943], Brunker, SW [0000-0001-6776-2550], Salzer, JJ [0000-0001-8483-603X], Wilkins, SM [0000-0003-3903-6935], Almaini, O [0000-0001-9328-3991], Bagley, MB [0000-0002-9921-9218], Berg, DA [0000-0002-4153-053X], Bhatawdekar, R [0000-0003-0883-2226], Bisigello, L [0000-0003-0492-4924], Buat, V [0000-0003-3441-903X], Burgarella, D [0000-0002-4193-2539], Calabrò, A [0000-0003-2536-1614], Casey, CM [0000-0002-0930-6466], Ciesla, L [0000-0003-0541-2891], Cleri, NJ [0000-0001-7151-009X], Cole, JW [0000-0002-6348-1900], Cooray, AR [0000-0002-3892-0190], Costantin, L [0000-0001-6820-0015], Croton, D [0000-0002-5009-512X], Ferguson, HC [0000-0001-7113-2738], Finkelstein, SL [0000-0001-8519-1130], Fujimoto, S [0000-0001-7201-5066], Gardner, JP [0000-0003-2098-9568], Gawiser, E [0000-0003-1530-8713], Giavalisco, M [0000-0002-7831-8751], Grazian, A [0000-0002-5688-0663], Grogin, NA [0000-0001-9440-8872], Hathi, NP [0000-0001-6145-5090], Hirschmann, M [0000-0002-3301-3321], Holwerda, BW [0000-0002-4884-6756], Huertas-Company, M [0000-0002-1416-8483], Hutchison, TA [0000-0001-6251-4988], Jogee, S [0000-0002-1590-0568], Juneau, S [0000-0002-0000-2394], Jung, I [0000-0003-1187-4240], Kartaltepe, JS [0000-0001-9187-3605], Kirkpatrick, A [0000-0002-1306-1545], Kocevski, DD [0000-0002-8360-3880], Koekemoer, AM [0000-0002-6610-2048], Lotz, JM [0000-0003-3130-5643], Lucas, RA [0000-0003-1581-7825], Magnelli, B [0000-0002-6777-6490], Matharu, J [0000-0002-7547-3385], Pérez-González, PG [0000-0003-4528-5639], Pirzkal, N [0000-0003-3382-5941], Rafelski, M [0000-0002-9946-4731], Rose, C [0000-0002-8018-3219], Seillé, LM [0000-0001-7755-4755], Somerville, RS [0000-0002-6748-6821], Straughn, AN [0000-0002-4772-7878], Tacchella, S [0000-0002-8224-4505], Vanderhoof, BN [0000-0002-8163-0172], Weiner, BJ [0000-0001-6065-7483], Wuyts, S [0000-0003-3735-1931], and Zavala, JA [0000-0002-7051-1100]

Subjects
similar-to 2, SIMILAR-TO 2, NEAR-INFRARED SPECTROSCOPY, COLLISION STRENGTHS, near-infrared spectroscopy, MASS-METALLICITY RELATION, FOS: Physical sciences, CHEMICAL-COMPOSITION, Galaxies and Cosmology, collision strengths, LY-ALPHA, atomic database, STAR-FORMING GALAXIES, MOSDEF SURVEY, mosdef survey, NEBULAR EMISSION, Astronomy and Astrophysics, mass-metallicity relation, star-forming galaxies, Astrophysics - Astrophysics of Galaxies, ATOMIC DATABASE, ly-alpha, nebular emission, Space and Planetary Science, 5101 Astronomical Sciences, Astrophysics of Galaxies (astro-ph.GA), chemical-composition, 51 Physical Sciences
Abstract

We present rest-frame optical emission-line flux ratio measurements for five $z>5$ galaxies observed by the JWST Near-Infared Spectrograph (NIRSpec) in the SMACS 0723 Early Release Observations. We add several quality-control and post-processing steps to the NIRSpec pipeline reduction products in order to ensure reliable relative flux calibration of emission lines that are closely separated in wavelength, despite the uncertain \textit{absolute} spectrophotometry of the current version of the reductions. Compared to $z\sim3$ galaxies in the literature, the $z>5$ galaxies have similar [OIII]$\lambda$5008/H$\beta$ ratios, similar [OIII]$\lambda$4364/H$\gamma$ ratios, and higher ($\sim$0.5 dex) [NeIII]$\lambda$3870/[OII]$\lambda$3728 ratios. We compare the observations to MAPPINGS V photoionization models and find that the measured [NeIII]$\lambda$3870/[OII]$\lambda$3728, [OIII]$\lambda$4364/H$\gamma$, and [OIII]$\lambda$5008/H$\beta$ emission-line ratios are consistent with an interstellar medium that has very high ionization ($\log(Q) \simeq 8-9$, units of cm~s$^{-1}$), low metallicity ($Z/Z_\odot \lesssim 0.2$), and very high pressure ($\log(P/k) \simeq 8-9$, units of cm$^{-3}$). The combination of [OIII]$\lambda$4364/H$\gamma$ and [OIII]$\lambda$(4960+5008)/H$\beta$ line ratios indicate very high electron temperatures of $4.1, Comment: Accepted for publication in AAS Journals. 14 pages, 6 figures, 3 tables

Published
2023

21. The VANDELS survey: a strong correlation between Ly α equivalent width and stellar metallicity at 3 ≤ z ≤ 5

Author

A. Calabrò, O. Cucciati, G. Zamorani, D. J. McLeod, Ross J. McLure, Nimish P. Hathi, Lucia Guaita, B. Garilli, James Dunlop, Johan P. U. Fynbo, Laura Pentericci, Mauro Giavalisco, Marco Castellano, Margherita Talia, Andrea Cimatti, Fergus Cullen, Adriano Fontana, M. Bolzonella, A. Saxena, Ricardo Amorín, Giovanni Cresci, A. C. Carnall, F. Mannucci, Michele Cirasuolo, Fabio Fontanot, Matt J. Jarvis, Lucia Pozzetti, Anton M. Koekemoer, Alice E. Shapley, ITA, USA, GBR, FRA, DEU, Cullen, F, McLure, RJ, Dunlop, JS, Carnall, AC, McLeod, DJ, Shapley, AE, Amorin, R, Bolzonella, M, Castellano, M, Cimatti, A, Cirasuolo, M, Cucciati, O, Fontana, A, Fontanot, F, Garilli, B, Guaita, L, Jarvis, MJ, Pentericci, L, Pozzetti, L, Talia, M, Zamorani, G, Calabro, A, Cresci, G, Fynbo, JPU, Hathi, NP, Giavalisco, M, Koekemoer, A, Mannucci, F, and Saxena, A

Subjects
Physics, education.field_of_study, Stellar population, 010308 nuclear & particles physics, astro-ph.GA, Metallicity, Population, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Spectral line, galaxies: high-redshift, Space and Planetary Science, 0103 physical sciences, Spectral fitting, galaxies: evolution, education, 010303 astronomy & astrophysics, Equivalent width, evolution [galaxies], high-redshift [galaxies]
Abstract

We present the results of a new study investigating the relationship between observed Ly α equivalent width (Wλ(Ly α)) and the metallicity of the ionizing stellar population ( Z⋆) for a sample of 768 star-forming galaxies at 3 ≤ z ≤ 5 drawn from the VANDELS survey. Dividing our sample into quartiles of rest-frame Wλ(Ly α) across the range $-58 \,\rm {\mathring{\rm A}} \lesssim$ Wλ(Ly α) $\lesssim 110 \,\rm {\mathring{\rm A}}$ , we determine Z⋆ from full spectral fitting of composite far-ultraviolet spectra and find a clear anticorrelation between Wλ(Ly α) and Z⋆. Our results indicate that Z⋆ decreases by a factor ≳ 3 between the lowest Wλ(Ly α) quartile (λ(Ly α) $\rangle =-18\,\rm {\mathring{\rm A}}$ ) and the highest Wλ(Ly α) quartile (λ(Ly α) $\rangle =24\,\rm {\mathring{\rm A}}$ ). Similarly, galaxies typically defined as Lyman alpha emitters (LAEs; Wλ(Ly α) $\gt 20\,\rm {\mathring{\rm A}}$ ) are, on average, metal poor with respect to the non-LAE galaxy population (Wλ(Ly α) $\le 20\,\rm {\mathring{\rm A}}$ ) with Z⋆non-LAE ≳ 2 × Z⋆LAE. Finally, based on the best-fitting stellar models, we estimate that the increasing strength of the stellar ionizing spectrum towards lower Z⋆ is responsible for ${\simeq}15{-}25{{\ \rm per\ cent}}$ of the observed variation in Wλ(Ly α) across our sample, with the remaining contribution ( ${\simeq}75{-}85{{\ \rm per\ cent}}$ ) being due to a decrease in the H I/dust covering fractions in low- Z⋆ galaxies.

Published
2020

22. CEERS Key Paper I: An Early Look into the First 500 Myr of Galaxy Formation with JWST

Author

Steven L. Finkelstein, Micaela B. Bagley, Henry C. Ferguson, Stephen M. Wilkins, Jeyhan S. Kartaltepe, Casey Papovich, L. Y. Aaron Yung, Pablo Arrabal Haro, Peter Behroozi, Mark Dickinson, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Aurélien Le Bail, Alexa M. Morales, Pablo G. Pérez-González, Denis Burgarella, Romeel Davé, Michaela Hirschmann, Rachel S. Somerville, Stijn Wuyts, Volker Bromm, Caitlin M. Casey, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Taylor A. Hutchison, Saurabh W. Jha, Shardha Jogee, Lisa J. Kewley, Allison Kirkpatrick, Arianna S. Long, Jennifer M. Lotz, Laura Pentericci, Justin D. R. Pierel, Nor Pirzkal, Swara Ravindranath, Russell E. Ryan, Jonathan R. Trump, Guang Yang, Rachana Bhatawdekar, Laura Bisigello, Véronique Buat, Antonello Calabrò, Marco Castellano, Nikko J. Cleri, M. C. Cooper, Darren Croton, Emanuele Daddi, Avishai Dekel, David Elbaz, Maximilien Franco, Eric Gawiser, Benne W. Holwerda, Marc Huertas-Company, Anne E. Jaskot, Gene C. K. Leung, Ray A. Lucas, Bahram Mobasher, Viraj Pandya, Sandro Tacchella, Benjamin J. Weiner, Jorge A. Zavala, Finkelstein, SL [0000-0001-8519-1130], Bagley, MB [0000-0002-9921-9218], Ferguson, HC [0000-0001-7113-2738], Wilkins, SM [0000-0003-3903-6935], Kartaltepe, JS [0000-0001-9187-3605], Papovich, C [0000-0001-7503-8482], Yung, LY [0000-0003-3466-035X], Haro, PA [0000-0002-7959-8783], Behroozi, P [0000-0002-2517-6446], Dickinson, M [0000-0001-5414-5131], Kocevski, DD [0000-0002-8360-3880], Koekemoer, AM [0000-0002-6610-2048], Larson, RL [0000-0003-2366-8858], Le Bail, A [0000-0002-9466-2763], Morales, AM [0000-0003-4965-0402], Pérez-González, PG [0000-0003-4528-5639], Burgarella, D [0000-0002-4193-2539], Davé, R [0000-0003-2842-9434], Hirschmann, M [0000-0002-3301-3321], Somerville, RS [0000-0002-6748-6821], Wuyts, S [0000-0003-3735-1931], Bromm, V [0000-0003-0212-2979], Casey, CM [0000-0002-0930-6466], Fontana, A [0000-0003-3820-2823], Fujimoto, S [0000-0001-7201-5066], Gardner, JP [0000-0003-2098-9568], Giavalisco, M [0000-0002-7831-8751], Grazian, A [0000-0002-5688-0663], Grogin, NA [0000-0001-9440-8872], Hathi, NP [0000-0001-6145-5090], Hutchison, TA [0000-0001-6251-4988], Jha, SW [0000-0001-8738-6011], Jogee, S [0000-0002-1590-0568], Kewley, LJ [0000-0001-8152-3943], Kirkpatrick, A [0000-0002-1306-1545], Long, AS [0000-0002-7530-8857], Lotz, JM [0000-0003-3130-5643], Pentericci, L [0000-0001-8940-6768], Pierel, JDR [0000-0002-2361-7201], Pirzkal, N [0000-0003-3382-5941], Ravindranath, S [0000-0002-5269-6527], Ryan, RE [0000-0003-0894-1588], Trump, JR [0000-0002-1410-0470], Yang, G [0000-0001-8835-7722], Bhatawdekar, R [0000-0003-0883-2226], Bisigello, L [0000-0003-0492-4924], Buat, V [0000-0003-3441-903X], Calabrò, A [0000-0003-2536-1614], Castellano, M [0000-0001-9875-8263], Cleri, NJ [0000-0001-7151-009X], Cooper, MC [0000-0003-1371-6019], Croton, D [0000-0002-5009-512X], Daddi, E [0000-0002-3331-9590], Dekel, A [0000-0003-4174-0374], Elbaz, D [0000-0002-7631-647X], Franco, M [0000-0002-3560-8599], Gawiser, E [0000-0003-1530-8713], Holwerda, BW [0000-0002-4884-6756], Huertas-Company, M [0000-0002-1416-8483], Jaskot, AE [0000-0002-6790-5125], Leung, GCK [0000-0002-9393-6507], Lucas, RA [0000-0003-1581-7825], Mobasher, B [0000-0001-5846-4404], Pandya, V [0000-0002-2499-9205], Tacchella, S [0000-0002-8224-4505], Weiner, BJ [0000-0001-6065-7483], Zavala, JA [0000-0002-7051-1100], and Apollo - University of Cambridge Repository

Subjects
epoch simulations flares, cosmology legacy survey, deblended dust emission, uv luminosity functions, ultra-deep field, hubble frontier fields, FOS: Physical sciences, Astronomy and Astrophysics, initial mass function, 5109 Space Sciences, space-telescope observations, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, similar-to 10, Astrophysics of Galaxies (astro-ph.GA), 51 Physical Sciences, high-redshift galaxies
Abstract

We present an investigation into the first 500 Myr of galaxy evolution from the Cosmic Evolution Early Release Science (CEERS) survey. CEERS, one of 13 JWST ERS programs, targets galaxy formation from z~0.5 to z>10 using several imaging and spectroscopic modes. We make use of the first epoch of CEERS NIRCam imaging, spanning 35.5 sq. arcmin, to search for candidate galaxies at z>9. Following a detailed data reduction process implementing several custom steps to produce high-quality reduced images, we perform multi-band photometry across seven NIRCam broad and medium-band (and six Hubble broadband) filters focusing on robust colors and accurate total fluxes. We measure photometric redshifts and devise a robust set of selection criteria to identify a sample of 26 galaxy candidates at z~9-16. These objects are compact with a median half-light radius of ~0.5 kpc. We present an early estimate of the z~11 rest-frame ultraviolet (UV) luminosity function, finding that the number density of galaxies at M_UV ~ -20 appears to evolve very little from z~9 to z~11. We also find that the abundance (surface density [arcmin^-2]) of our candidates exceeds nearly all theoretical predictions. We explore potential implications, including that at z>10 star formation may be dominated by top-heavy initial mass functions, which would result in an increased ratio of UV light per unit halo mass, though a complete lack of dust attenuation and/or changing star-formation physics may also play a role. While spectroscopic confirmation of these sources is urgently required, our results suggest that the deeper views to come with JWST should yield prolific samples of ultra-high-redshift galaxies with which to further explore these conclusions., 41 pages, 20 figures, 6 tables, submitted to ApJL. Key results in Figures 13-15, discussed in Sections 7 and 8

Published
2022
Full Text
View/download PDF

23. The ALPINE–ALMA [C ii] Survey: Multiwavelength Ancillary Data and Basic Physical Measurements

Author

Faisst A. L., Schaerer D., Lemaux B. C., Oesch P. A., Fudamoto Y., Cassata P., Bethermin M., Capak P. L., Fevre O. L., Silverman J. D., Yan L., Ginolfi M., Koekemoer A. M., Morselli L., Amorin R., Bardelli S., Boquien M., Brammer G., Cimatti A., Dessauges-Zavadsky M., Fujimoto S., Gruppioni C., Hathi N. P., Hemmati S., Ibar E., Jones G. C., Khusanova Y., Loiacono F., Pozzi F., Talia M., Tasca L. A. M., Riechers D. A., Rodighiero G., Romano M., Scoville N., Toft S., Vallini L., Vergani D., Zamorani G., Zucca E., Faisst, AL, Schaerer, D, Lemaux, BC, Oesch, PA, Fudamoto, Y, Cassata, P, Bethermin, M, Capak, PL, Le Fevre, O, Silverman, JD, Yan, L, Ginolfi, M, Koekemoer, AM, Morselli, L, Amorin, R, Bardelli, S, Boquien, M, Brammer, G, Cimatti, A, Dessauges-Zavadsky, M, Fujimoto, S, Gruppioni, C, Hathi, NP, Hemmati, S, Ibar, E, Jones, GC, Khusanova, Y, Loiacono, F, Pozzi, F, Talia, M, Tasca, LAM, Riechers, DA, Rodighiero, G, Romano, M, Scoville, N, Toft, S, Vallini, L, Vergani, D, Zamorani, G, Zucca, E, Faisst, A. L., Schaerer, D., Lemaux, B. C., Oesch, P. A., Fudamoto, Y., Cassata, P., Bethermin, M., Capak, P. L., Fevre, O. L., Silverman, J. D., Yan, L., Ginolfi, M., Koekemoer, A. M., Morselli, L., Amorin, R., Bardelli, S., Boquien, M., Brammer, G., Cimatti, A., Dessauges-Zavadsky, M., Fujimoto, S., Gruppioni, C., Hathi, N. P., Hemmati, S., Ibar, E., Jones, G. C., Khusanova, Y., Loiacono, F., Pozzi, F., Talia, M., Tasca, L. A. M., Riechers, D. A., Rodighiero, G., Romano, M., Scoville, N., Toft, S., Vallini, L., Vergani, D., Zamorani, G., Zucca, E., Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astrophysics, 01 natural sciences, Interstellar medium, Astrophysics::Solar and Stellar Astrophysics, Galaxy processes, 010303 astronomy & astrophysics, Stellar evolution, Physics, education.field_of_study, Star formation, Astrophysics::Earth and Planetary Astrophysics, Galaxy evolution, Galactic and extragalactic astronomy, Galaxy photometry, Stellar masses, Interstellar medium wind, Galaxy winds, Stellar winds, Far infrared astronomy, Stellar wind, Galaxy wind, Population, Doubly ionized oxygen, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Galaxy formation and evolution, education, Astrophysics::Galaxy Astrophysics, Galaxy processe, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Stellar masse, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract

We present the ancillary data and basic physical measurements for the galaxies in the ALMA Large Program to Investigate C+ at Early Times (ALPINE) survey - the first large multi-wavelength survey which aims at characterizing the gas and dust properties of 118 main-sequence galaxies at redshifts 4.4 < z < 5.9 via the measurement of [CII]-emission at 158 micro-meter (64% at >3.5$\sigma$) and the surrounding far-infrared (FIR) continuum in conjunction with a wealth of optical and near-infrared data. We outline in detail the spectroscopic data and selection of the galaxies as well as the ground- and space-based imaging products. In addition, we provide several basic measurements including stellar masses, star formation rates (SFR), rest-frame ultra-violet (UV) luminosities, UV continuum slopes ($\beta$), and absorption line redshifts, as well as H-alpha emission derived from Spitzer colors. We find that the ALPINE sample is representative of the 4 < z < 6 galaxy population selected by photometric methods and only slightly biased towards bluer colors ($\Delta\beta$ ~ 0.2). Using [CII] as tracer of the systemic redshift (confirmed for one galaxy at z=4.5 out of 118 for which we obtained optical [OII]$\lambda$3727A emission), we confirm red shifted Ly-alpha emission and blue shifted absorption lines similar to findings at lower redshifts. By stacking the rest-frame UV spectra in the [CII] rest-frame we find that the absorption lines in galaxies with high specific SFR are more blue shifted, which could be indicative of stronger winds and outflows., Comment: 48 pages, 33 figures, 7 tables (including Appendix), accepted for publication in ApJS

Published
2020

Catalog

Books, media, physical & digital resources
See catalog results