Stellar Mass and 3.4µm M/L Ratio Evolution of Brightest Cluster Galaxies in COSMOS since 1.0
We investigate the evolution of star formation rates (SFRs), stellar masses, and M/L ratios of brightest cluster galaxies (BCGs) in the COSMOS survey since to determine the contribution of star formation to the growth-rate of BCG stellar mass over time. Through the spectral energy distribution (SED) fitting of the GALEX, CFHT, Subaru, Vista, Spitzer, and Herschel photometric data available in the COSMOS2015 catalog, we estimate the stellar mass and SFR of each BCG. We use a modified version of the iSEDfit package to fit the SEDs of our sample with both stellar and dust emission models, as well as constrain the impact of star formation history assumptions on our results. We find that in our sample of COSMOS BCGs, star formation evolves similarly to that in BCGs in samples of more massive galaxy clusters. However, compared to the latter, the magnitude of star formation in our sample is lower by 1 dex. Additionally, we find an evolution of BCG baryonic mass-to-light ratio () with redshift which is consistent with a passively aging stellar population. We use this to build upon Wen et al.’s low-redshift relation, quantifying a correlation between and M to z 1. By comparing our results to BCGs in Sunyaev–Zel’dovich and X-ray-selected samples of galaxy clusters, we find evidence that the normalization of star formation evolution in a cluster sample is driven by the mass range of the sample and may be biased upwards by cool cores.
Subject headings:galaxies: clusters: general – galaxies: elliptical and lenticular, cD – galaxies: star formation
Dominating the luminosity and stellar mass in the central region of galaxy clusters, and influencing their evolution, are brightest cluster galaxies (BCGs). These massive ellipticals occupy a narrower distribution of position-velocity space in relation to other cluster members (Lauer et al., 2014), indicating a relaxed state within the parent cluster. However, they do not represent the same population (Von Der Linden et al., 2007) as other ellipticals in the cluster or the field. One unique characteristic of BCGs is their extended light profiles (e.g. Oemler, 1976; Graham et al., 1996), indicating a rich merger history (e.g Bernardi et al., 2007; Liu et al., 2008). Additionally, BCGs exhibit larger sizes and luminosities than predicted from cluster luminosity functions (e.g. Loh & Strauss, 2006; Shen et al., 2014).
Recent observations of star-forming BCGs has led to a revision of their formation scenario over the past decade. The original model derived from theoretical predictions (e.g. Merritt, 1984) and observations (e.g. Stott et al., 2010, 2011) postulates a BCG formation mechanism in which the original gas and stellar content of a BCG formed in the initial matter density peaks (Treu et al., 2005). The rest of its constituent stars form via in situ processes rapidly before , which evolve passively to the present day. This is contrasted by semi-analytical models in which BCGs grow in stellar mass by a factor of three from to the present day (De Lucia & Blaizot, 2007). The newest models exhibit a factor of two growth over the same redshift range (e.g. Shankar et al., 2015), in which BCG stellar mass is accumulated through many minor mergers (e.g. Naab et al., 2009; Edwards & Patton, 2012), which has led to greater agreement between observations and models (Lidman et al., 2012; Lin et al., 2013). Whether this merger-driven era dominates mass growth is still under investigation, as minor mergers are not 100% efficient in the delivery of their gas supply or stars (Liu et al., 2009; Burke & Collins, 2013; Liu et al., 2015).
One important problem is to constrain the role of star formation in BCG growth, since this process may contribute significant stellar mass to BCGs in the case of wet mergers, or in the case of cool-core clusters, if condensed intracluster medium (ICM) gas fuels a significant buildup of stellar mass (O’Dea et al., 2008). While the mass growth of BCGs at is believed to be substantial (with estimates placing stellar mass growth in BCGs doubling or tripling), there is considerable disagreement over how much of that mass growth is ongoing at (e.g. McIntosh et al., 2008; Tonini et al., 2012; Bai et al., 2014; Oliva-Altamirano et al., 2014; Inagaki et al., 2015; Bellstedt et al., 2016), and whether new formed stars are contributing substantially to that growth (Gozaliasl et al., 2016). Selection effects due to different selection criteria (e.g. whether the sample is optically or X-ray limited) may play a role in driving this disparity of results(Burke et al., 2000), as well as different observed wavelengths, or assumptions such as selection of initial mass function (IMF) or evolution models to constrain stellar population.
In this paper, we seek to constrain the contribution of BCG stellar mass growth made by in situ star formation in a sample of X-ray-selected, low-mass (M = M) galaxy clusters in the COSMOS field. We compare our findings with BCGs in higher-mass cluster samples obtained using both X-ray and Sunyaev–Zel’dovich (SZ) effect selection criteria to better understand the impact of cluster environment and sample selection on the estimation of the evolution of BCG star formation. By modeling BCG spectral energy distributions (SEDs) using far-UV (FUV) to far-IR (FIR) observations, we can better constrain the old and young stellar populations in a self-consistent manner that considers stellar populations obscured by IR-emitting dust. We also can consider several stellar population models, and constrain the impact of these models on our results. By estimating specific star formation rates (sSFRs) in BCGs over a wide redshift range, we better constrain when star formation took place and whether or not star formation in different cluster samples evolves similarly.
In §2 we discuss target selection criteria and sample completeness. We review the archival data used in the SED fitting procedure in §3 and discuss the data reduction and SED fitting software in §4. We discuss the results in §6. Finally, we summarize our results and future prospects in §7. We use the CDM standard cosmological parameters of = 70 Mpc km s, = 0.3, and = 0.7.
2. Sample Selection
In order to build our sample from uniform observations and selection method, we select clusters in the COSMOS X-ray group and cluster catalog (Finoguenov et al., 2007; George et al., 2011) between , with greater than 30 spectroscopically confirmed or high probability ( 0.5) cluster members. We choose a cutoff of 30 members to select well-detected clusters as have been previously studied in COSMOS (Delaye et al., 2014), and are more populated and massive than the known protoclusters in COSMOS which have 5-10 members (e.g. Diener et al., 2015). These redshift and angular size limits correspond to a contiguous comoving volume of 7 10 Mpc. To identify the BCG within each cluster, we estimate the stellar mass of all group members with 0.5 using the SED fitting procedure described in Section 4 and select the group member with the highest estimated stellar mass. The mass difference between BCG and second most massive group galaxy is shown in Fig. 1. Throughout the paper, we also plot a comparison sample of massive group members with estimated stellar masses greater than 75% of the stellar mass of the BCG identified for that group.
This yields an initial sample of 44 BCGs with no selection for star formation rate (SFR) activity. Their parent clusters span the range of log(m/M) 12.9-14.3, as determined by the cluster X-ray luminosity (Finoguenov et al., 2007), and calibrated via gravitational lensing measurement of the COSMOS field (Leauthaud et al., 2010; George et al., 2011). We note that COSMOS is biased toward a denser region of sky than a random patch (Finoguenov et al., 2007), with two large overdensities: at z 0.3 (Masters et al., 2011) and the ‘COSMOS Wall’ at z 0.73 (Scoville et al., 2013; Iovino et al., 2016). We address the potential impact of these overdensities in Section 5 by running our analysis with objects in range of these overdensities in redshift space excluded.
COSMOS groups and clusters were originally detected by identifying extended sources on the scale of 32”; and 64” using the wavelet analysis of Vikhlinin et al. (1998), in the Chandra and 1.4 Ms observations of the COSMOS field. Once identified, George et al. (2011) ran a red-sequence finding algorithm to identify an optical counterpart within a projected distance of 500 kpc of the X-ray center. A galaxy is included as a member galaxy using a Bayesian analysis of galaxy properties such as location with respect to cluster or group center, redshift error, and relative number of field and cluster or group galaxies (see Section 4 of George et al., 2011).
Our BCG sample requires no completion correction as the COSMOS X-ray group member catalog is complete down to K = 24 mag and F184W = 24.2 mag (corresponding to an approximate stellar mass of M 10 M at z = 1; George et al. 2011). However, group mass is limited to out to , which may bias our group selection to higher masses at high redshift (George et al., 2011). Stellar mass estimates used in the COSMOS X-ray group catalog are estimated via SED fitting of galaxies with 3 detections in the K band, using Bruzual & Charlot (2003) stellar population models with a Chabrier (2003) IMF. Two targets, COSMOS CLJ100028.3+024103 and COSMOS CL J095824.0+024916, had updated photometric redshifts above z = 1 in the more recent COSMOS2015 catalog (Laigle et al., 2016).
3. COSMOS Data
To accurately derive stellar masses and SFRs for each BCG, we use FUV–FIR observations of the COSMOS field (Scoville et al., 2007). COSMOS is a multi-wavelength survey that observed a 2 sq. deg. field centered at R.A.(J2000) = 10:00:28.600, decl.(J2000) = +02:12:21.00 from the X-ray to the radio, with publicly available multi-wavelength data available in the COSMOS2015 catalog (Laigle et al., 2016). A short review of each observation set is below; for further details of the data reduction in COSMOS2015, see Laigle et al. (2016). The following photometry has been corrected for photometric and systematic offsets as detailed in Eq. 9 in Laigle et al. (2016). For observations from GALEX FUV-Spitzer IRAC4, we also correct for Milky Way foreground extinction using a Galactic reddening of = 3.1 (Morrissey et al., 2007) and values from the Schlegel et al. (1998) dust maps.
For our SED fitting, we use errors which include the observational error reported in the COSMOS2015 catalog as well as the absolute calibration uncertainty unique to each telescope. For GALEX NUV and FLUX flux errors, we include a 10 uncertainty111https://asd.gsfc.nasa.gov/archive/galex/FAQ/counts_background.html. Subaru photometric calibration is accurate to within 0.02 mag (Taniguchi et al., 2015), therefore we include a systematic error of 2%. For the Canada–France–Hawaii Telescope (CFHT) u*, we err on the side of caution and use the 5% error from worst-quality data of the original observations of the COSMOS field (Capak et al., 2007). According to the /VIRCAM User Manual,222Doc. No. VIS-MAN-ESO-06000-0002 photometry is accurate to within 3-5% and so we include a 5% error in addition to the observational error for data from /VIRCAM filters. absolute flux calibration is considered accurate to within 3% (Van Dyk et al., 2013), so we add an additional 3% to our final IRAC errors. Most data used here are upper limits defined by the sensitivity of the original surveys of the COSMOS fields, the PACS Evolutionary Probe (PEP; Lutz et al., 2011) and the Herschel Multi-tiered Extragalactic Survey (HerMES; Oliver et al., 2012). For the handful of detections in our sample, we adopt the 10% systematic uncertainty term used in Fogarty et al. (2017).
To constrain the degree of unobscured star formation, we use GALEX (Martin et al., 2005) FUV and NUV band point-spread function (PSF)-fit photometric magnitudes presented in the COSMOS2015 catalog (for details see Zamojski et al., 2007). GALEX observes a 12 circular field of view through a 50 cm diameter Richey–Chretien telescope. To measure FUV and NUV magnitudes, Zamojski et al. (2007) use a PSF-fitting routine using band observations as a prior to minimize blending effects due to GALEX’s FWHM of 5″.
3.2. Canada–France–Hawaii Telescope (CFHT)
We use COSMOS2015 CFHT/MegaPrime (Aune et al., 2003; Boulade et al., 2003) magnitudes to constrain the blue and NUV rest-frame emission. The COSMOS field was observed in queue mode with a consistent PSF across all observations, to a depth of m 26.4 and seeing of 0.9″. For further details, see Capak et al. (2007).
To constrain the optical continuum of each BCG, we retrieve Subaru/Suprime-Cam optical magnitudes from the COSMOS2015 catalog in five broad filters (, , ) and 11 medium filters (IA427, IA464, IA484, IA505, IA527, IA574, IA624, IA679, IA738, IA767, and IA827). The Subaru observations with the worst resolution are from the IA464 filter with a PSF FWHM of 189, which is still sufficient enough to resolve the BCGs in our sample. All observations reach a depth of m or deeper. For further details, see Taniguchi et al. (2007, 2015).
NIR observations are an important constraint for the old stellar population which dominates the emission and stellar mass of BCGs. We retrieve and -band (Dalton et al., 2006; Emerson et al., 2006) observations taken with VIRCAM (Sutherland et al., 2015) during the UltraVISTA-DR2 survey (McCracken et al., 2012). For UltraVISTA, the COSMOS field was observed with and filters down to limiting magnitude of 25.3, 24.9, and 24.6 respectively with a median FWHM of 06.
Additional observations of the old stellar population are available through NIR to MIR observations taken by the Spitzer Space Telescope (Werner et al., 2004). We include archival data from Spitzer’s Infrared Array Camera (IRAC) 3.6, 4.5, 5.7, and 7.9 µm channels (For more information, see Fazio et al., 2004). IRAC observes 52 x 52 degree fields with PSF widths 16, 16, 18, and 19 for bands IRAC1 to IRAC4 respectively. IRAC magnitudes in COSMOS2015 are measured from observations taken as part of the SPLASH (Steinhardt et al., 2014) and S-COSMOS surveys (Sanders et al., 2007) to a 3 depth of of 25.5, 25.5, 23.0, and 22.9 for IRAC1-4 respectively. We also include Multiband Imaging Photometer (MIPS, Rieke et al., 2004) 24µm fluxes originally presented in Le Floc’h et al. (2009) to a 3 depth of 80 Jy. To account for blending, photometry from and observations were used as a prior during the source extraction of the 3.6 µm image (Laigle et al., 2016). Each successive IRAC filter used the adjacent shorter wavelength image as a prior out to 24 .
The FIR is an important regime for observing the re-radiated energy from dust surrounding obscured star forming regions. We use the Herschel Space Observatory (Pilbratt et al., 2010) Photoconductor Array Camera and Spectrometer (PACS) (Poglitsch et al., 2010) in the green (100 µm) and red (160 µm) bands as well as the Spectral and Photometric Imaging Receiver (SPIRE) 250 µm and 350 µm bands. While the large beam size at 250 and 350 µm (181, 249 respectively) guarantees blending, all but three targets at 350µm and all but six at 250µm are non-detections and the fluxes that are detected have low signal-to-noise ratio (S/N) and therefore modest constraining power on the SED fits. PACS observations were taken as part of PEP (Lutz et al., 2011) to a 3 depth of 5 and 10.2 mJy for 100 and 160 µm bands respectively. SPIRE observations originate from HerMES (Oliver et al., 2012) and reach a 3 depth of 8.1 and 10.7 mJy at 250 and 350 respectively. The MIPS 24 image of the COSMOS field was used as a prior during source extraction from the FIR images (Laigle et al., 2016).
4.1. SED Construction
SEDs were composed of photometry taken from GALEX, Subaru, Vista, Spitzer, and Herschel in the COSMOS2015 public catalog, so as to maximize coverage of UV-through-IR flux. Of these, 34 had GALEX NUV and/or FUV detections, 43 had full Spitzer/IRAC detections with the 44th (COSMOS CLJ100013.0+023519) detected in only IRAC1-3, 18 were detected in MIPS 24 µm, and 9 with Herschel PACS or SPIRE detections. Therefore, every BCG in the final catalog has rest-frame -band through MIR detections, with limiting magnitudes out to 350 µm.
We note that our study differentiates itself from that of Gozaliasl et al. (2016, 2018), who study a sample of 407 X-ray-selected groups, including those detected in the COSMOS field in George et al. (2011) and Finoguenov et al. (2007), in terms of how we estimate stellar properties of cluster galaxies and in terms of our treatment of galaxies comparably massive to the BCG. These studies cite results from either Ilbert et al. (2013) or Laigle et al. (2016), which do not incorporate FIR photometry into estimates of the SFR. Our fits take into account both the observed UV flux of the young stellar population and the flux absorbed by dust and re-emitted in the FIR, and therefore measure the total SFR of each system. Furthermore, by selecting only those COSMOS clusters with at least 30 members, and by taking into account comparably massive galaxies in clusters which lack a clearly dominant galaxy, we limit ourselves to rich systems that are comparable to higher-mass cluster analogs and account for the effects of potentially ambiguous BCG selection.
4.2. SED Fitting
SEDs were fit using a modified version of iSEDfit (Moustakas et al., 2013; Moustakas, 2017). iSEDfit is a Bayesian SED fitting tool that uses a grid of synthetic SEDs generated using a set of input priors to estimate the posterior probability distribution of parameters of the stellar population emitting an observed SED. We used the modified version of this tool described in Fogarty et al. (2017) in order to take into account both the stellar and dust emission observed in the NUV-through-IR SEDs of our sample.
A detailed description of iSEDfit is available in Appendix A of Moustakas et al. (2013). iSEDfit takes a synthetic stellar population, IMF, and dust attenuation law, and creates a grid of synthetic SEDs that randomly sample the parameter space of metallicity, A, emission line ratios, and the parameters governing the star formation history (SFH) using user-defined prior distributions. For each BCG, we assume a Salpeter (1955) IMF. In order to determine the extent to which our results depend on the parameterization of the SFH, we tested two SFH parameterizations, a one-component model and a two-component model. The former consists of an exponentially decaying SFH with a decay constant between 0.6 and 60 Gyr sampled logarithmically. The latter consists of an exponentially decaying SFH with a decay constant between 0.3 and 1.5 Gyr, and for half of the models in our grid we incorporated an exponentially decaying starburst at present time. For either model, the age of the BCG was allowed to vary between 6 and 9 Gyr if the BCG was at , or between 4 and 6 Gyr if the BCG was at . These age priors were chosen to ensure that model stellar populations do not exceed the age of the universe at the redshift of the galaxy, while still ensuring an old stellar component. This enables us to fit SEDs of both quiescent (nominally ‘red and dead’) and star-forming BCGs. Our choices of stellar population model and parameter space are given in Table 1.
|Stellar Population Model|
|Synthetic Stellar Population||Bruzual & Charlot (2003)|
|Initial Mass Function||Salpeter (1955)|
|Attenuation Law||Calzetti et al. (2000)|
|Dust Emission||Draine & Li (2007)|
|Model Parameter Space Constraints|
|Parameter Name||Minimum Value||Maximum Value||Sampling Interval|
|Age,||4 Gyr (6 Gyr)||6 Gyr (9 Gyr)||Linear|
|Decay Timescale,||0.6 Gyr||60.0 Gyr||Logarithmic|
|Age,||4 Gyr (6 Gyr)||6 Gyr (9 Gyr)||Linear|
|Decay Timescale,||0.3 Gyr||1.5 Gyr||Linear|
|Burst Age,||Gyr||5.0 Gyr||Logarithmic|
|Burst Decay Percentage||0.01||0.99||Linear|
|Burst Mass Percentage||0.0015||0.85||Logarithmic|
|PAH Abundance Index||0.10||4.58||Linear|
Minimum and maximum values for ages inside parentheses apply to BCGs at , while those outside the parentheses apply to BCGs at .
Burst parameters were sampled logarithmically, since their qualitative effect on the model SED of the galaxy occurs on order-of-magnitude scales. The exception to this is the burst decay percentage, which is one minus the amplitude of current star formation activity relative to the amplitude of the burst years ago.
Draine & Li (2007) model parameter sampling intervals were chosen based on the model parameter distributions of the template spectra.
The Draine & Li (2007) treats dust in a galaxy as consisting of two components. The first component consists of a fraction of the dust is exposed to a power-law distribution of starlight intensity, ranging from to , while the second component consists of the remainder of the dust, and is only exposed to a starlight intensity . The quantities and are unitless measures of intensity relative to the ambient local radiation field.
The relative likelihood that each model SED is the observed SED is determined by calculating , where is the reduced chi square value for the model compared to the data. By randomly sampling the model grid, weighted by the relative likelihood, iSEDfit recovers the posterior probability distribution of the model SEDs, and therefore the probability distribution of the physical stellar parameter input (Moustakas et al., 2013).
Dust emission is incorporated into the synthetic SED grid, allowing us to take full advantage of the MIR and FIR data available from Spitzer, and Herschel. SED fits incorporating observations of the IR dust emission are preferable to those that do not since they reduce the degeneracy between A and the SFR in fits to dusty star-forming systems. Following the prescription in Fogarty et al. (2017), we used the dust emission templates in Draine & Li (2007). The choice dust model parameter space is given in Table 1. The dust emission component of each synthetic SED was normalized such that the total energy re-emitted by the dust equals the total energy absorbed via attenuation of the synthetic stellar spectrum.
Our choice of dust model is the Calzetti et al. (2000) attenuation law for dusty starburst galaxies. As the galaxies we study are typically dust poor, the choice of dust model has a limited impact on the SED fit. Furthermore, as was shown in Fogarty et al. (2017), even vigorously star-forming BCGs have relatively modest A values, and the choice of attenuation law does not significantly affect the outcome of UV–FIR SED fitting.
Model grids consisting of models were constructed for both the one-component and two-component SFH parameterizations. These model grids were shifts to the observer frame for each galaxy studied in order to produce synthetic photometry for each fit. Parameters were sampled either linearly or logarithmically in the intervals listed in Table 1.
5.1. BCG Stellar Population Evolution
We present the BCG SFR and sSFR as a function of redshift in Figure 2 . Unless otherwise specified, we report results obtained with the single-component SFH parameterization throughout. SFRs and sSFRs for the individual BCGs are presented in the Appendix, along with best-fit SEDs. We demonstrate SFR is weakly dependent on redshift, within our errors, as is the sSFR. We compare our results to those obtained in McDonald et al. (2016), who estimated mean SFRs and sSFRs in redshift bins for BCGs in an SZ-selected sample of clusters with masses between . We also defined four redshifts bins, , , and , and calculated the -weighted mean SFRs and sSFRs for each bin. These are reported in Figure 2 with color-coded shaded regions with vertical limits depicting the 1 credible interval for the mean. For all plots we include the BCG from each group as well as any massive (M/M 0.75) group members. We notice no discernible difference in the trends for SFR, sSFR, or M between these two subsamples.
|log SFR (One-component SFH) [M yr]|
|log SFR (One-component SFH, All Large Gals.)|
|log SFR (One-component SFH, Structure Excised)|
|log SFR (Two-component SFH)|
|log sSFR (One-component SFH) [yr]|
|log sSFR (One-component SFH), All Large Gals.)|
|log sSFR (One-component SFH, Structure Excised)|
|log sSFR (Two-component SFH)|
Includes both BCGs and galaxies within the stellar mass of their respective BCG.
Binned results obtained when excluding BCGs in the overdense structures at and
Redshift binned results are reported in Table 2. SFR declines by approximately one order of magnitude from z 1 to the present day. Across all redshift bins, we find a typical BCG SFR of 0.1–1 M yr. The SFR trends are similar whether we consider the one-component or two-component SFH, although SFRs and sSFRs are about 0.5 dex lower when measured using the two-component SFH (given the uncertainties, however; this difference is marginally significant).
Finally, we considered the impact of excising clusters in the overdense redshift regions discussed in Section 2. These results are given in Table 2 as well. The overdensities at z and extend in redshift space between and respectively (Masters et al., 2011; Iovino et al., 2016), resulting in our excluding 12 clusters from bins 1-3. The overall shift in our results is well within our uncertainties.
The mean sSFR decreases by about 1 dex across the redshift range in our study. In Figure 2 we show that, as redshift increases to 1, the typical sSFR for a BCG in our sample grows from per Gyr to per Gyr. Since the catalog we use probes masses uniformly across the range of redshifts we study, our results in Figure 2 suggest some growth in the weighted mean sSFR may occur at , which would be consistent with McDonald et al. (2016) even after accounting for the order of magnitude offset between our sample and their SZ-selected sample. We find that across our redshift range, the sample we study probes the mass range 11.2 M - 12.5 M relatively uniformly, as seen in Figure 3.
Finally, we examined the redshift evolution of the BCG mass-to-light ratio. These results are presented in Figure 4. Studies such as Fraser-McKelvie et al. (2014) and Wen et al. (2013) use the – W1 luminosity relationship to estimate stellar masses of BCGs at and 0.35 respectively. However, further estimation of BCG stellar masses at higher redshifts requires estimates of the evolution of with redshift. Therefore, we computed W1 rest frame luminosities by estimating the best-fit model W1 photometry in iSEDfit. This band is sensitive to the population of old stars which compose the majority of the BCG’s stellar mass, in addition to being less sensitive to recent star formation and dust than other bands. We fit a linear model to the ratio versus redshift using the least-squares method in Hogg et al. (2010). The resulting redshift evolution of the stellar mass (M) to light (L (3.4)) ratio is:
Across this range of redshift space, the ratio changes by a factor of 1.3.
Wen et al. (2013) find ratios of 1.5-2 for some massive early-type galaxies with , consistent with an extrapolation to low redshift from Eq. 1 (Fig. 4). The nearest contaminant in the NIR which could effect our result is the 3.3 polycyclic aromatic hydrocarbon (PAH) emission feature, which will not be detected since the rest-frame W1 central wavelengths span 1.8–2.5 µm across the redshifts observed in our sample.
5.2. An Active Galactic Nucleus Outlier in COSMOS CL J100035.2+020346
The fit with the highest corresponds to COSMOS CL J100035.2+020346’s BCG (R.A. = 150.148794; decl. = 2.060569), with a of 7.6. Upon examination of its SED (see Appendix), its positive NIR slope indicates the possible presence of an active galactic nucleus (AGN) component. We test this hypothesis by comparing the IRAC band fluxes of this target with the criteria set by Donley et al. (2012) as well as the obscured AGN models of Lacy et al. (2004, 2007). This BCG does not satisfy the Donley et al. (2012) criterion of an IR AGN; however the ratio of IRAC band flux ratios do match well with the model from Polletta et al. (2008) for an elliptical galaxy hosting an obscured AGN contributing 0-20 of the total galaxy NIR output. No radio counterpart is detected in the COSMOS catalogs, nor in the soft X-ray Chandra observations. However, this target is detected in the hard X-ray band (2–7 keV) by Elvis et al. (2009) at a S/N of 4.49, and a corresponding L of 6.29 10 ergs s. We believe this target is an active X-ray AGN with minimal dust content surrounding the black hole.
6.1. Contribution of star formation to BCG mass growth
Our typical sSFR values are 10 across all redshift bins, indicative of a doubling time of yr, and thus a stellar growth rate due to star formation on the order of 1% Gyr across the redshift range studied. After accounting for stellar mass loss and recycling, this rate is corrected to 0.4% Gyr (e.g. Kennicutt et al., 1994; Brinchmann et al., 2004).
Our results are closest to the lower bound of McIntosh et al. (2008)’s 1.4-6.4%/Gyr growth rate and consistent with Oliva-Altamirano et al. (2014)’s lack of significant change at lower redshift (). However, our results indicate an order of magnitude less growth than from Bai et al. (2014) and Inagaki et al. (2015), who used red sequence and X-ray luminosity selected BCGs. Inagaki et al. (2015) fit SZ-effect selected BCGs using only SDSS magnitudes via kcorrect and NewHyperZ, using Bruzual & Charlot (2003) stellar population models and a Chabrier IMF. Our result is consistent with their lower limit of 2%, but not their upper limit of 14%. They also noted that NewHyperZ yielded higher masses than their kcorrect models and that their selection of early-type galaxy models may have influenced the result. Bai et al. (2014) used the GALFIT luminosity of their targets combined with the M/L ratio given by the Maraston et al. (2009) luminous red galaxy models. This difference in stellar and M/L ratio assumptions may be contributors to our different results.
We also find that our sample is significantly more quiescent than the sample of groups presented in Gozaliasl et al. (2018), since they find that the mean SFR in their sample can account for as much as 45% of the growth rate of brightest group galaxies. We suspect that this result is driven by star-forming BGGs in either the lower-mass or galaxy-poorer halos in their sample, which is consistent with the median SFR in their sample being consistent with our mean across redshift space. Taken together, these results suggest distinct evolutionary histories between BCGs and BGGs that can be distinguished in halos with total masses of M M. Alternatively, the degeneracy between SFR and in SEDs without MIR and FIR constraints may result in the overestimation of the SFR in a minority of cases.
This work’s mean sSFR is higher than that of 9.42 in Cooke et al. (2016), who investigated the Sloan Giant Arcs Survey (SGAS) and Cluster Lensing and Supernova Survey with (CLASH) samples. This is expected, as their estimators only measured unobscured rates while our inclusion of IR upper limits constrains the star formation obscured by dust as well as the un-obscured component.
As noted above, this is an order of magnitude less growth than in McDonald et al. (2016), which diverges further from our results at higher redshift as wet merger-driven stellar mass growth drives higher SFRs. Using detections from the SPT, McDonald et al. (2016)’s sample probes the most massive BCGs across the southern hemisphere, each more massive than our BCG sample. We believe the discrepancy in stellar mass growth rate is due to their mass selection requiring a more aggressive merger-driven mass growth in their past in order to reach their observed masses, an aggressive growth rate not required by our lower mass sample.
6.1.1 Comparison with X-Ray and SZ-selected Cluster Samples
We use available archival data from three other X-ray-selected BCG studies in order to provide a larger sample to test whether BCG star formation is typical of other massive galaxies: the ACCEPT survey (Cavagnolo et al., 2009), the BCGs studied by Mittal et al. (2015), and the CLASH (Postman et al., 2012). Of these samples, the CLASH BCGs occupy a stellar mass and redshift range most like the present sample, having masses above 10 and a redshift range of . However, the CLASH survey selected massive ( keV), morphologically symmetrical (ellipticity ) clusters, and so contains more massive clusters than COSMOS and a large fraction () of cool cores (Postman et al., 2012). Meanwhile, the ACCEPT clusters overlap with both the COSMOS and the CLASH cluster masses. Stellar mass and SFRs were calibrated to a common Salpeter IMF for comparison.
The ACCEPT survey selected 239 X-ray clusters in the temperature range keV and the bolometric luminosity range erg s, spanning redshifts (Cavagnolo et al., 2009). SFRs and stellar masses of ACCEPT cluster BCGs were measured in Hoffer et al. (2012). We include sSFR values for BCGs with SFRs estimated using 70 Spitzer MIPS observations or NUV GALEX observations from Hoffer et al. (2012).
The CLASH survey (Postman et al., 2012) observed 25 galaxy clusters, of which 20 were selected by X-ray temperature and morphology. Five more strongly lensing clusters with Einstein radii 35; were also included. Fogarty et al. (2015) and Donahue et al. (2015) independently investigate the star formation characteristics of the CLASH sample.
As seen in Fig. 5, the sSFR of BCGs decreases as a function of stellar mass for the overall comparison sample. The behavior of actively star-forming BCGs is consistent on average with the star-forming main sequence at the mean redshift of all of the samples(Noeske et al., 2007; Lee et al., 2015). This behavior is not evident in the individual samples we plot, however, since each sample occupies a relatively narrow range of stellar masses. Furthermore, while the ACCEPT and CLASH samples overlap the main-sequence star forming range, our COSMOS sample is systematically more quiescent than what would be predicted by the star-forming main sequence, while the Mittal et al. (2015) sample is systematically more active.
We suspect individual BCGs have evolved off the star-forming main sequence, so the apparent trend between stellar mass and sSFR evident when comparing the BCGs from these different X-ray-selected samples is consistent with BCG star formation being driven by processes in the halo external to the BCG. One noteworthy aspect of Fig. 5 is that the BCGs in the X-ray samples appear to straddle the star forming main sequence, which suggests a link between the halo-driven fueling process in BCGs and field massive ellipticals. It is also likely that whether or not the mean star formation behavior of a sample of BCGs is consistent with the star forming main sequence depends on how the sample selects for cool cores. The morphology selection of CLASH increases the incidence of cool-core clusters in the sample, thereby increasing the incidence of cooling-induced BCG star formation, which likely contributes to why the COSMOS sample is systematically more quiescent than the CLASH sample despite occupying the same stellar mass bin.
The tendency of COSMOS BCGs toward quiescence may be a function of the cluster’s mass. Figure 6 displays sSFR vs. cluster M for the COSMOS, ACCEPT, and CLASH samples, as well as the SZ-selected sample in McDonald et al. (2016). Cluster masses were estimated for COSMOS and ACCEPT by converting X-ray luminosities to using the scaling relation in Pratt et al. (2009). Masses for CLASH were estimated through a combination of strong and weak lensing (Merten et al., 2015).
These results suggest BCG evolution may be affected by cluster mass, although it is possible that different effects might dominate at different redshifts. First, we consider the COSMOS and SPT samples. The COSMOS sample is both significantly more quiescent and lower mass than the SPT sample. The majority of the high-sSFR BCGs in the SPT sample occur at high redshift, while the sSFR characteristics of the COSMOS sample are still systematically lower at low redshift (log sSFR yr as opposed to to yr). McDonald et al. (2016) cite merger driven star-formation in young cluster environments at high redshift as driving the evolution of star formation in their sample. The discrepancy between our findings and those of McDonald et al. (2016) may be explained by the hypothesis that evolution observed in McDonald et al. (2016) is merger driven at . In the high redshift bins, more massive clusters will have undergone more cluster mergers, which at high redshift may serve as a gas delivery mechanism to drive star formation. As a result, a high-cluster mass sample like the SPT sample would have BCGs with higher sSFRs than a low-cluster mass sample like COSMOS at high redshifts.
The CLASH and ACCEPT samples, meanwhile, occupy the full range of cluster masses and BCG sSFRs bracketed by the COSMOS and SPT samples. These X-ray-selected samples are lower redshift ( for CLASH and for the ACCEPT clusters used in this paper, as opposed to for the SPT sample), and therefore we expect star formation to be induced by cooling. Taken together, they show that the BCG sSFR depends on mass in X-ray-selected clusters at low to moderate redshifts in the sense that star formation can be more vigorous as cluster mass increases, but need not be (while the ACCEPT BCGs show a trend between sSFR and M, we suspect the bolometric luminosity-derived masses in ACCEPT may be biased by cool cores, and implying this trend may actually be reflective of the correlation between BCG star formation and the presence of cool cores). A plausible physical explanation at lower redshifts is that the larger sSFRs of BCGs in more massive clusters have the potential to be supported by proportionally larger reservoirs if these BCGs are in the cores of cool-core clusters.
6.2. Evolution of with Redshift
Previous studies at low redshift (e.g. Wen et al., 2013; Fraser-McKelvie et al., 2014) found a correlation between stellar mass and rest-frame W1 luminosity density at . This correlation will evolve with redshift as the W1 band observations include emission from a younger and brighter stellar population. Therefore, we measured the evolution of the ratio across a redshift range between 0.2 and 1.0 using our COSMOS dataset. Our estimated ratio of at is consistent with the high-mass end of the relationship in Wen et al. (2013). For a 10 galaxy, Wen et al. (2013) predict a ratio of 10. Since the masses used in their results were estimated from colors calibrated assuming a Chabrier (2003) IMF, it matches our results given the 0.2 dex offset between the Chabrier (2003) and Salpeter (1955) IMFs.
The slope in our overall relationship is consistent with the passive evolution of a stellar population becoming redder over time, following a Bruzual & Charlot (2003) evolutionary track from 3 to 10 Gyr old. Our measurement of the ratio is consistent with the body of results supporting dry-merger-driven stellar mass growth in BCGs (e.g., De Lucia & Blaizot, 2007; Whiley et al., 2008; Vulcani et al., 2016). In particular, our results from the COSMOS sample imply that the addition of new mass to a BCG does not change its mass-to-light ratio, so the stellar population of cannibalized galaxies must be a similar age to the existing population in the galaxy. Since observations indicate that BCG masses grow by a factor of 2 between = 0.9 and 0.2, stars from early-type stellar populations must accrete onto the BCGs without triggering star formation (Lidman et al., 2012, 2013; Rodriguez-Gomez et al., 2017). Our findings also align with observations of the evolution of the ratio out to , which also imply passive BCG evolution (van der Marel & van Dokkum, 2007).
We examined the role of star formation in the stellar mass growth of BCGs in low-mass clusters at intermediate redshifts by fitting the SEDs of 44 BCGs below in the COSMOS survey. By using publicly available archival data from the FUV to FIR, we estimated SFR and M across four redshift bins (, , and ). By comparing our estimates with similar work examining more massive clusters in the literature, we conclude the following:
BCG SFR weakly declines with redshift from to the present day. We find evidence that the sSFRs of BCGs in low-mass clusters evolve at least down to , but that at all redshifts these galaxies are systematically more quiescent than their higher-mass cluster counterparts.
An evolution of the baryonic M/L ratio with redshift is observed and fit. This redshift-dependent correlation provides an extension of that found by Wen et al. (2013), previously limited to .
Star formation plays very little role in BCG mass growth in the COSMOS sample. Our estimates for the contribution of star formation to BCG stellar mass at ( per Gyr) is consistent with or below the low end of similar estimates in the literature.
While we find evidence for evolving SFRs in COSMOS BCGs, when compared to the massive SZ-limited sample of McDonald et al. (2016), our sample is systematically more quiescent across redshift bins. We suspect that the processes governing the evolution of star formation are the same in these homogeneously selected samples of clusters, but the magnitude of star formation is a selection effect. By comparing with both this sample and X-ray selected samples of clusters at lower redshifts (which have a greater tendency than either COSMOS or SZ-selected samples to select clusters that have formed cool cores), we are led to suspect that this effect is as function of how samples select cluster mass and ICM dynamical state.
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Fit parameters for individual COSMOS BCGs are presented in Table 3. We report the median SFR and sSFR and 1 uncertainties obtained for each galaxy. Values for are reported for the best-fitting model in the Monte Carlo grid for each BCG. Best-fit model spectra for each BCG are shown in Figure 7.
|COSMOS CL J100045.6+013926||0.21||1.98|
|COSMOS CL J100201.2+021330||0.825||2.68|
|COSMOS CL J100013.6+021230||0.18||1.83|
|COSMOS CL J100005.7+021211||0.923||1.22|
|COSMOS CL J100056.8+021225||0.36||1.1|
|COSMOS CL J100109.1+021637||0.11||1.69|
|COSMOS CL J100051.5+021648||0.862||1.2|
|COSMOS CL J100139.8+022548||0.13||2.68|
|COSMOS CL J095951.4+014049||0.38||2.66|
|COSMOS CL J100013.9+022249||0.4||1.74|
|COSMOS CL J095833.6+022056||0.992||0.93|
|COSMOS CL J095907.2+022358||0.351||1.41|
|COSMOS CL J100027.4+022123||0.22||1.84|
|COSMOS CL J100021.8+022328||0.21||2.95|
|COSMOS CL J095847.9+022410||0.355||2.84|
|COSMOS CL J095931.8+022654||0.36||2.25|
|COSMOS CL J100016.0+023850||0.707||2.04|
|COSMOS CL J095941.6+023129||0.741||1.14|
|COSMOS CL J095940.6+023603||0.256||2.41|
|COSMOS CL J100056.0+022834||0.38||1.51|
|COSMOS CL J100138.5+023514||0.1||1.94|
|COSMOS CL J095957.1+023506||0.69||1.29|
|COSMOS CL J100013.0+023519||0.64||2.85|
|COSMOS CL J100028.3+024103||0.35||2.81|
|COSMOS CL J100111.9+014037||0.523||0.91|
|COSMOS CL J095924.4+014623||0.12||1.85|
|COSMOS CL J095901.5+024740||0.49||3.21|
|COSMOS CL J095824.0+024916||0.34||1.56|
|COSMOS CL J100020.7+023153||0.87||1.22|
|COSMOS CL J100027.0+023321||0.5||2.02|
|COSMOS CL J100043.2+014607||0.34||1.48|
|COSMOS CL J100049.6+014923||0.302||3.6|
|COSMOS CL J100139.3+015051||0.39||1.8|
|COSMOS CL J095805.4+015256||0.342||1.03|
|COSMOS CL J100217.7+015601||0.52||2.68|
|COSMOS CL J100128.6+015958||0.82||1.23|
|COSMOS CL J100147.3+020314||0.53||1.89|
|COSMOS CL J100035.2+020346||0.986||0.94|
|COSMOS CL J100200.6+020405||0.521||1.82|
|COSMOS CL J100141.0+015904||0.3||1.81|
|COSMOS CL J100139.2+022435||0.809||1.0|
|COSMOS CL J095945.1+023622||0.324||3.09|
|COSMOS CL J100031.5+015108||0.735||7.6|
|COSMOS CL J100135.3+024617||0.44||1.29|
Uncertainties denote the 1 credible intervals for each value.
Best-fit sSFRs based on iSEDfit.