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J/ApJ/834/101    Keck/MOSFIRE spectroscopy of ZFOURGE galaxies    (Tran+, 2017)

ZFIRE: similar stellar growth in Hα-emitting cluster and field galaxies at z∼2. Tran K.-V.H., Alcorn L.Y., Kacprzak G.G., Nanayakkara T., Straatman C., Yuan T., Cowley M., Dave R., Glazebrook K., Kewley L.J., Labbe I., Martizzi D., Papovich C., Quadri R., Spitler L.R., Tomczak A. <Astrophys. J., 834, 101-101 (2017)> =2017ApJ...834..101T (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, IR ; Spectra, infrared ; Redshifts ; Photometry, H-alpha Keywords: galaxies: evolution; galaxies: starburst; galaxies: star formation Abstract: We compare galaxy scaling relations as a function of environment at z∼2 with our ZFIRE survey where we have measured Hα fluxes for 90 star-forming galaxies selected from a mass-limited (log(M*/M)>9) sample based on ZFOURGE. The cluster galaxies (37) are part of a confirmed system at z=2.095 and the field galaxies (53) are at 1.9<z<2.4; all are in the COSMOS legacy field. There is no statistical difference between Hα-emitting cluster and field populations when comparing their star formation rate (SFR), stellar mass (M*), galaxy size (reff), SFR surface density (Σ(Hαstar)), and stellar age distributions. The only difference is that at fixed stellar mass, the Hα-emitting cluster galaxies are log(reff)∼0.1 larger than in the field. Approximately 19% of the Hα emitters in the cluster and 26% in the field are IR-luminous (LIR>2x1011L). Because the luminous IR galaxies in our combined sample are ∼5 times more massive than the low-IR galaxies, their radii are ∼70% larger. To track stellar growth, we separate galaxies into those that lie above, on, or below the Hα star-forming main sequence (SFMS) using ΔSFR(M*)=±0.2dex. Galaxies above the SFMS (starbursts) tend to have higher Hα SFR surface densities and younger light-weighted stellar ages than galaxies below the SFMS. Our results indicate that starbursts (+SFMS) in the cluster and field at z∼2 are growing their stellar cores. Lastly, we compare to the (SFR-M*) relation from Rhapsody-G cluster simulations and find that the predicted slope is nominally consistent with the observations. However, the predicted cluster SFRs tend to be too low by a factor of ∼2, which seems to be a common problem for simulations across environment. Description: Here we combine Hα emission from our ZFIRE survey (Nanayakkara+ 2016, J/ApJ/828/21) with galaxy properties from the ZFOURGE survey (Straatman+ 2016, J/ApJ/830/51) and IR luminosities from Spitzer to track how galaxies grow at z∼2. ZFIRE is a near-IR spectroscopic survey with MOSFIRE on Keck I where targets are selected from ZFOURGE, an imaging survey that combines deep near-IR observations taken with the FourStar Imager at the Magellan Observatory with public multi-wavelength observations, e.g., Hubble Space Telescope (HST) imaging from CANDELS (Grogin+ 2011ApJS..197...35G). The Keck/MOSFIRE spectroscopy was obtained on observing runs in 2013 December and 2014 February. A total of eight slit masks were observed in the K-band (1.93-2.38um). We also observed two masks in the H-band covering 1.46-1.81um. Objects: ----------------------------------------------------------------------- RA (ICRS) DE Designation(s) ----------------------------------------------------------------------- 10 00 18.38 +02 14 58.0 galaxy cluster = [SLG2012] Galaxy Cluster ----------------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 83 90 Galaxy properties
See also: VII/265 : COSMOS Morphological Catalog (V1.1) (Tasca+ 2009) J/ApJ/830/51 : FourStar galaxy evolution survey (ZFOURGE) (Straatman+, 2016) J/ApJ/828/21 : ZFIRE v1.0 data release (Nanayakkara+, 2016) J/ApJ/817/118 : SFR-M* relation from ZFOURGE (Tomczak+, 2016) J/ApJS/219/15 : Morphologies of z=0-10 galaxies with HST data (Shibuya+, 2015) J/ApJS/218/33 : Spitzer-CANDELS catalog within 5 deep fields (Ashby+, 2015) J/ApJS/214/24 : 3D-HST+CANDELS catalog (Skelton+, 2014) J/ApJS/212/18 : An atlas of UV-to-MIR galaxy SEDs (Brown+, 2014) J/ApJS/203/24 : Structural param. of galaxies in CANDELS (van der Wel+, 2012) J/ApJ/682/985 : FIREWORKS photometry of GOODS CDF-S (Wuyts+, 2008) J/ApJ/655/51 : HDFS IRAC observations of 2<z<3.5 galaxies (Wuyts+, 2007) : ZFIRE home page : ZFOURGE home page Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 4 I4 --- ZFIRE [237/9922] ZFIRE source identifier (1) 6- 10 I5 --- ZFOURGE [912/14346] ZFOURGE source identifier (1) 12- 20 F9.5 deg RAdeg Right Ascension in decimal degrees (J2000) 22- 28 F7.5 deg DEdeg Declination in decimal degrees (J2000) 30- 35 F6.4 --- zsp [1.9/2.4] Spectroscopic redshift 37- 41 F5.2 10-20W/m2 FHa [0.4/11.2] Observed Hα flux, 10-17erg/s/cm2 43- 46 F4.2 10-20W/m2 e_FHa [0.05/0.3] Uncertainty in FHa 48- 52 F5.2 [Lsun] LIR [8.7/12.3]? Log of IR luminosity (2) 54- 58 F5.2 [Msun] Mstar [8.9/11] Log of stellar mass 60- 62 F3.1 mag Av [0/1.6] Extinction 64- 66 F3.1 [Gyr] t [7.9/9.4] Log of stellar age (3) 68- 71 F4.1 Msun/yr SFR [1/84] Hα based star formation rate (4) 73- 75 F3.1 --- n [0.3/8]? Sersic index 77- 79 F3.1 arcsec Reff [0.1/0.9]? Effective radius 81- 83 I3 --- Pflag [-99/2]? Quality of profile fit (0=good fit) (5)
Note (1): Galaxy identification numbers from ZFIRE (Nanayakkara+ 2016, J/ApJ/828/21) and ZFOURGE (Straatman+ 2016, J/ApJ/830/51). We include only galaxies with spectroscopic redshift quality flag of Q_z=3 (Nanayakkara+ 2016, J/ApJ/828/21) and 1.9<zsp<2.4. Cluster members (37 galaxies) have 2.08<zsp<2.12 (Yuan+ 2014ApJ...795L..20Y). Note (2): In our analysis of IR-luminous vs. low-IR systems, we select IR-luminous galaxies using log(LIR/Lsun)>11.3. Note (3): Stellar age in units of Gyr and based on SED fitting with FAST (Kriek et al., 2009ApJ...700..221K). Note (4): Hα star formation rates in units of Msun/yr and based on dust-corrected Hα fluxes (Eq. 2; see Section 2.4). Note (5): Quality of profile fit used to measure the Sersic index, n, and the effective radius, Reff as follows: -99 = not fit; 0 = good fit; 1 = fair fit; 2 = questionable fit.
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 02-Jun-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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