We present stellar population properties of early-type galaxies from the VIMOS Public Extragalactic Redshift Survey (VIPERS) based on the spectral measurements of ∼ 4000 galaxies with stellar masses from 10^{10} to 10^{12} {[M_{☉}]} in the redshift range 0.4 < z < 1.0. We quantify relations between their age, stellar metallicity, duration of star burst, and stellar mass. We compare the properties of VIPERS intermediate redshift galaxies with galaxies found in the Local Universe

Fritz, Alexander

GARILLI, BIANCA MARIA ROSA

Malek, Katarzyna

Pollo, Agnieszka

SCODEGGIO, MARCO

Siudek, Małgorzata

OA@INAF - Istituto Nazionale di Astrofisica

2016Publication Year2020-05-13T16:54:20ZAcceptance in OA@INAFVIPERS: Stellar population properties of early-type galaxiesTitleþÿ S i u d e k ,   M aB g o r z a t a ;   M a l e k ,   K a t a r z y n a ;   G A R I L L I ,   B I A N C A   M A R I A   R O S A ;  SCODEGGIO, MARCO; Fritz, Alexander; et al.Authorshttp://hdl.handle.net/20.500.12386/24813HandlePROCEEDINGS OF THE POLISH ASTRONOMICAL SOCIETYSeries3NumberVIPERS: Stellar population properties ofearly-type galaxiesMa lgorzata Siudek1, Katarzyna Malek2, Bianka Garilli3, Marco Scodeggio3,Alexander Fritz3, Agnieszka Pollo2·4 and The VIPERS Team51. Center for Theoretical Physics, Al. Lotnikow 32/46, 02-668 Warsaw, Poland;2. National Center for Nuclear Research, ul. A. Soltana 7, 05-400 Otwock, Poland;3. INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica Milano, via Bassini 15, 20133Milano, Italy;4. Astronomical Observatory of the Jagiellonian University, Orla 171, 30-001 Cracow,Poland;5. The VIPERS Team coauthors are presented at the end of this proceedingsWe present stellar population properties of early-type galaxies from the VIMOSPublic Extragalactic Redshift Survey (VIPERS) based on the spectral measure-ments of ∼ 4000 galaxies with stellar masses from 1010 to 1012 [M] in the redshiftrange 0.4 < z < 1.0. We quantify relations between their age, stellar metallicity,duration of star burst, and stellar mass. We compare the properties of VIPERSintermediate redshift galaxies with galaxies found in the Local Universe.1 IntroductionTracing ages and chemical abundances of stellar populations of early-type galaxies(ETGs) at different redshifts as a function of their mass puts additional constraintson mechanisms leading to the global suppression of star formation and the build-upof the quiescent galaxy population. According to the ”downsizing” scenario (Cowieet al., 1996; Cimatti et al., 2006), the evolution of galaxies is controlled by their mass,i.e. stars are formed earlier and faster in massive galaxies, which, as a consequence,complete their star formation at higher redshifts than lower mass galaxies. The ar-guments in favor for the downsizing scenario were delivered by a number of authors(e.g. Renzini, 2006; Pozzetti et al., 2010; Fritz et al., 2014). The analysis of physicalproperties of high-mass red sequence galaxies at z ≤ 0.7 shows that their evolutionis passive (e.g. Choi et al., 2014; Gallazzi et al., 2014). Unfortunately, studies ofproperties of stellar populations at intermediate redshift (i.e z ≥ 0.5) are still lim-ited due to the necessity of deep spectroscopy in the rest-frame parts of the spectrawhere absorption features sensitive to age and metallicity are located. VIMOS PublicExtragalactic Redshift Survey (VIPERS, Guzzo et al., 2014), an European SouthObservatory (ESO) Large Program, has the potential to change this situation, pro-viding a dataset of nearly 100,000 distant galaxies at redshift 0.5 < z < 1.2 (five toten times larger than any other datasets ever assembled at this redshift range).2 DataWe present results for a sample of ∼ 4,000 ETGs selected from the VIPERS survey.Our analysis is based on the VIPERS internal Data Release version 5. We have246 ? PTA Proceedings ? June, 2016 ? vol. 3 pta.edu.pl/proc/v3p246VIPERS: Stellar population properties of early-type galaxiesselected 3,991 ETGs using the bimodal U-V color criterion with the evolving cut in(U-V) color (Fritz et al., 2014), and with additional criteria to obtain a reliable anduniform sample (for a detailed description we refer the reader to Siudek et al., 2016).We have divided this set of rest-frame galaxy spectra into a 2-dimensional grid ofredshift-stellar mass bins: 6 redshift bins from 0.4 to 1.0 with δz=0.1, and 7 stellarmass bins from log(Mstar) = 10.00 up to 11.25 [M] with δlog(Mstar) = 0.25 dex, andone additional bin 11.25 < log(Mstar) < 12.00 [M], as the sample is less numerous inthe high stellar mass range. In each bin the rest-frame spectra were co-added using anaverage combination and a median scaling computed in a wavelength region between4010 and 4600Å. We consider only composite spectra of more than 20 single spectra,since, according to our tests, this limit allows to obtain a satisfactory signal-to-noise(S/N) ratio to measure spectral features used in this paper. Finally, for 32 compositespectra of early-type galaxies from the redshift range 0.4 < z < 1.0 with stellar massbetween 1010 and 1012[M], we have calculated spectral indicators: the 4000 Å break(D4000) (Balogh et al., 1999), and an absorption strength of high-order Balmer lineHδ at 4101Å (HδA) (Worthey & Ottaviani, 1997; for a detailed description we referthe reader to Siudek et al., 2015). Our cosmological framework assumes the densityparameter Ωm = 0.25, cosmological constant ΩΛ = 0.75, and reduced Hubble constanth70 = H0/(70 kms−1Mpc−1).3 Method and resultsWe have estimated the mean look-back time, stellar metallicity, and duration of burstadopting the approach proposed by Gallazzi et al. (2005). We have compared thestrengths of the spectral features (HδA and D4000) to the measurements made on agrid of synthetic spectra based on Bruzual & Charlot (2003) models. To create alibrary of synthetic spectra in the stellar synthesis modeling code we have used thefollowing initial conditions: (1) initial mass function from Chabrier (2003), (2) Padova1994 stellar evolutionary tracks, (3) high-resolution spectral library (STELIB), (4) therange of metallicities from sub- to super-solar (Z = 0.004, 0.008, 0.02, and 0.05), (5)star formation scenario with a single stellar burst of length between 0.1 ≤ τ ≤ 1 Gyrs(6) the range of ages from 1 up to 10 Gyrs since the beginning of the burst.The comparison of the strengths of the absorption features in the observed VIPERSstacked spectra with those obtained for a library of templates allows us to build theprobability density functions (PDFs) of physical properties of stellar populations,such as the look-back time, the metallicity, and the length of the burst (see Fig. 1).Following Gallazzi et al. (2005), the PDF is defined by the distribution of a givenparameter with the weights w = exp(−χ2/2 ), where χ2 is based on the measurementerrors of all the models in the library. Finally, we have established the mean valuesof parameters with errors corresponding to 1σ.The spectral indicators used to characterize the ETGs properties (D4000 and HδA)are well known as a good galaxy age indicators (e.g. Balogh et al., 1999; Kauffmannet al., 2003). The strength of D4000 depends strongly on metallicity, while HδAdepends on the α/Fe ratio, and therefore it may affect the age derivation of ellipticalgalaxies. However, Gallazzi et al. (2014) have shown that there is no indication ofa bias in the estimation of ages if only age indicators were used (D4000, Hβ, andHδA+HγA). The look-back times for VIPERS ETGs, estimated from these twospectroscopic features, stay in agreement with each other for each stellar mas bin (seeTab. 1). The obtained look-back time–mass relation or ETGs since z ∼ 1 is alsopta.edu.pl/proc/v3p246 PTA Proceedings ? June, 2016 ? vol. 3 ? 247Ma lgorzata Siudek, et al.4000(a) Look-back time.(b) Stellar metallicity.(c) Duration of star burst.Fig. 1: Distribution of physical properties of stellar populations (look-back time, stellarmetallicity, and duration of star burst) based on D4000 (three left panels) and HδAmeasurements (three right panels) of VIPERS ETGs. The dashed lines correspondto the probability density function.248 ? PTA Proceedings ? June, 2016 ? vol. 3 pta.edu.pl/proc/v3p246VIPERS: Stellar population properties of early-type galaxiesD4000 HδAMstar Look-back time σAge Look-back time σAge[M] [Gyr] [Gyr] [Gyr] [Gyr]10.00 < log(Mstar) < 10.25 7.80 1.08 7.57 1.1610.25 < log(Mstar) < 10.50 8.48 1.30 9.08 0.6610.50 < log(Mstar) < 10.75 8.81 1.27 9.47 1.0610.75 < log(Mstar) < 11.00 9.00 1.10 9.81 0.5711.00 < log(Mstar) < 11.25 9.53 1.35 9.86 1.1011.25 < log(Mstar) < 12.00 8.82 1.95 10.39 0.85Table 1: Mean look-back time estimated from the strength of D4000 and HδA indifferent stellar mass bins for our ETGs sample.consistent with results of Moresco et al. (2010) and Thomas et al. (2010) (see Fig. 2).Following Gallazzi et al. (2014) we have estimated the slope for the age-mass relationfor 0.6 < z < 0.8 (0.130 +/- 0.116), which is perfectly matched with slope observed forlocal galaxies (0.112+/-0.098) (Gallazzi et al., 2006). Distributions of the metallicityand the duration of the star burst do not reveal favoring values when comparing thestrength of the 4000Å break of VIPERS ETGs with the models (see left panel of Fig.1b, and 1c). However, if we take into consideration the distribution of HδA, which isnot so sensitive to the mean stellar metallicity, we find that galaxies with metallicityclose to the solar metallicity and the length of burst τ = 0.1 dominate the VIPERSETGs sample at 0.4 < z < 1.0 in all stellar mass bins. Our estimated length ofthe burst (τ ∼ 0.1) has been also observed before for local ETGs (Moresco et al.,2011). Gallazzi et al. (2006) have shown that metallicities for local ETGs vary in therange −0.2 < log(Z/Z) < 0.2. Comparing to their results, we have found that theVIPERS ETGs in the redshift range 0.4 < z < 1.0 have stellar metallicity consistentwith local quiescent galaxies, which implies no evolution in this parameter since z ∼ 1.However, we note that the estimation of the metallicity based on age-sensitive indicesonly, may be biased low (Gallazzi et al., 2014).4 ConclusionsWe have estimated the look-back time of VIPERS ETGs based on stellar populationsynthesis models of Bruzual & Charlot (2003), using the mean values of D4000 andHδA for VIPERS composite spectra. Our results show that 4000Å break alone isnot sufficient to determine the physical parameters of stellar population, such asthe metallicity or the length of the burst. However, the usage of both indicators(D4000 and HδA) allows to estimate stellar populations properties. From the spectralanalysis, we have found that:• The look-back time increases with the increasing stellar mass since z ∼ 1. Thisresult confirms the downsizing scenario, as massive galaxies have older stellarpopulation than the less massive ones.• The mean difference in age between high- and low-mass galaxies in our sampleis around 2 Gyr (between stellar mass ∼1.5·1010 and ∼1.2·1011 [M]).• Both D4000 and HδA are good age indicators and we do not find any evidencefor a bias in their look-back time estimation.pta.edu.pl/proc/v3p246 PTA Proceedings ? June, 2016 ? vol. 3 ? 249Ma lgorzata Siudek, et al.10.2 10.4 10.6 10.8 11.0 11.2 11.4log(Mstar)8.08.59.09.510.010.5log(t look−back/yr)0.6 < z < 0.8Fig. 2: Look-back time – stellar mass relation for redshift range 0.6 < z < 0.8. Thedashed line corresponds to linear fit.• A slope obtained from the linear regression fit of the look-back time – stellarmass relation is consistent with the same slope derived for local ETGs.• Our estimated length of the burst (τ ∼ 0.1) and metallicity close to the so-lar metallicity has been observed also for local, passively evolved ETGs, whatimplies no evolution in these parameters since z ∼ 1.VIPERS intermediate ETGs have stellar properties consistent with passive evolutionhypothesis. Star formation history of VIPERS ETGs wil be described in more detailin Siudek at el., 2016.Acknowledgements. We acknowledge the crucial contribution of the ESO stafffor the management of service observations. MS, AP, KM, and JK have beensupported by the National Science Centre (grants UMO-2012/07/B/ST9/04425 andUMO-2013/09/D/ST9/04030), the Polish-Swiss Astro Project.ReferencesBalogh, M. 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VIPERS: Stellar population properties of early-type galaxies

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VIPERS: Stellar population properties of early-type galaxies

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