Stellar and Total Mass in Early-Type Lensing Galaxies

Ferreras, Ignacio; Saha, Prasenjit; Williams, Liliya L. R.

doi:10.1086/429995

Cited by 81 publications

(133 citation statements)

References 29 publications

(34 reference statements)

Supporting

Mentioning

120

Contrasting

Order By: Relevance

“…Are we seeing part of a tidal tail? We estimated the stellar mass in galaxies G and X using the observed magnitudes and colors from CASTLeS 2 and standard population-evolution models, using the method described in Ferreras et al (2005), which yields $5 ; 10 11 M for G and $5 ; 10 10 M for X. The former is roughly half the total lensing mass, while the latter is roughly half the mass of the substructure.…”

Section: The Galaxy Lens Mg J0414+053mentioning

confidence: 99%

See 1 more Smart Citation

Meso‐Structure in Three Strong‐lensing Systems

Saha

Williams

Ferreras

2007

ApJ

Self Cite

View full text Add to dashboard Cite

We map substructure in three strong-lensing systems having particularly good image data: the galaxy lens MG J0414+053 and the clusters SDSS J1004+411 and ACO 1689. Our method is to first reconstruct the lens as a pixelated mass map and then subtract off the symmetric part (in the galaxy case) or a projected Navarro-Frenk-White profile (for the cluster lenses). In all three systems we find extended irregular structures, or meso-structures, having of order 10% of the total mass. In J0414+053, the meso-structure suggests a tidal tail connecting the main lens with a nearby galaxy; however, this interpretation is tentative. In the clusters, the identification of meso-structure is more secure, especially in ACO 1689, where two independent sets of lensed images imply very similar meso-structure. In all three cases, the meso-structures are correlated with galaxies but much more extended and massive than the stellar components of single galaxies. Such extended structures cannot plausibly persist in such high-density regions without being mixed; the crossing times are too short. The meso-structures therefore appear to be merging or otherwise dynamically evolving systems.

show abstract

Section: The Galaxy Lens Mg J0414+053mentioning

confidence: 99%

“…Figure 9 shows these galaxies. We have not attempted a population-evolution model, but a very rough extrapolation from Ferreras et al (2005) indicates a few times 10 12 M in stellar mass, much less than the mesostructure. The meso-structure does, however, correlate with the galaxies, as Figure 10 shows.…”

Section: The Cluster Aco 1689mentioning

confidence: 99%

Meso‐Structure in Three Strong‐lensing Systems

Saha

Williams

Ferreras

2007

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…The composite populations are obtained from the stellar population synthesis models of Bruzual & Charlot (2003), taking a Chabrier (2003) IMF. A wide range of ages and metallicities are considered (see Ferreras et al 2005 for details). Even though the inherent degeneracies with broadband photometry prevent us from extracting ages and metallicities, we can nevertheless determine the M/L ratio with acceptable uncertainty.…”

Section: Measuring Stellar Massesmentioning

confidence: 99%

Mapping the Distribution of Luminous and Dark Matter in Strong Lensing Galaxies

et al. 2007

Self Cite

View full text Add to dashboard Cite

Abstract. We present the distribution of luminous and dark matter in a set of strong lensing (early-type) galaxies. By combining two independent techniques -stellar population synthesis and gravitational lensing -we can compare the baryonic and dark matter content in these galaxies within the regions that can be probed using the images of the lensed background source. Two samples were studied, extracted from the CASTLES and SLACS surveys. The former probes a wider range of redshifts and allows us to explore the mass distribution out to ∼ 5R e . The high resolution optical images of the latter (using HST/ACS) are used to show a pixellated map of the ratio between total and baryonic matter. We find dark matter to be absent in the cores of these galaxies, with an increasing contribution at projected radii R > ∼ Re . The slopes are roughly compatible with an isothermal slope (better interpreted as an adiabatically contracted NFW profile), but a large scatter in the slope exists among galaxies. There is a trend suggesting most massive galaxies have a higher content of dark matter in the regions probed by this analysis.

show abstract

“…Gladders et al 1998;Stanford et al 1998;Barrientos & Lilly 2003;Ferreras et al 2005). However, a fundamental feature of earlytype formation in the standard LCDM model is that stellar mass that eventually ends up in present-day early-type galaxies is not entirely contained in early-type systems at high redshift.…”

Section: Introductionmentioning

confidence: 99%

Identifying the progenitor set of present-day early-type galaxies: a view from the standard model

Kaviraj

Devriendt

Ferreras³

et al. 2009

A&A

View full text Add to dashboard Cite

We present a comprehensive theoretical study, using a semi-analytical model within the standard LCDM framework, of the photometric properties of the progenitors of present-day early-type galaxies in the redshift range 0 < z < 1. We explore progenitors of all morphologies and study their characteristics as a function of the luminosity and local environment of the early-type remnant at z = 0. In agreement with previous studies, we find that, while larger early-types are generally assembled later, their luminosity-weighted stellar ages are typically older. In dense cluster-like environments, ∼70 percent of early-type systems are "in place" by z = 1 and evolve without interactions thereafter, while in the field the corresponding value is ∼30 percent. Averaging across all environments at z ∼ 1, less than 50 percent of the stellar mass which ends up in early-types today is actually in early-type progenitors at this redshift, in agreement with recent observational work. The corresponding value is ∼65 percent in clusters, due to faster morphological evolution in such dense environments. We develop probabilistic prescriptions which provide a means of including spiral (i.e. non early-type) progenitors at intermediate and high redshifts, based on their luminosity and optical colours. For example, we find that, at intermediate redshifts (z ∼ 0.5), large (M V < −21.5), red (B − V > 0.7) spirals have ∼75-95 percent chance of being an early-type progenitor, while the corresponding probability for large blue spirals (M B < −21.5, B − V < 0.7) is ∼50-75 percent. The prescriptions developed here can be used to address, from the perspective of the standard model, the issue of "progenitor bias", whereby the exclusion of late-type progenitors in observational studies can lead to inaccurate conclusions regarding the evolution of the early-type population over cosmic time. Finally, we explore the correspondence between the true "progenitor set" of the present-day early-type population -defined as the set of all galaxies that are progenitors of present-day early-types regardless of their morphologies -and the frequently used "red-sequence", defined as the set of galaxies within the part of the colour-magnitude space which is dominated by early-type objects. We find that, while more massive members (M V ≤ −21) of the "red sequence" trace the progenitor set reasonably well, the relationship breaks down at fainter luminosities (M V ≥ −21). Thus, while the results of recent observational studies which exploit the red sequence are valid (since they are largely restricted to massive galaxies), more care should be taken when deeper observations (which will probe fainter luminosities) become available in the future.

show abstract

Stellar and Total Mass in Early-Type Lensing Galaxies

Cited by 81 publications

References 29 publications

Meso‐Structure in Three Strong‐lensing Systems

Meso‐Structure in Three Strong‐lensing Systems

Mapping the Distribution of Luminous and Dark Matter in Strong Lensing Galaxies

Identifying the progenitor set of present-day early-type galaxies: a view from the standard model

Contact Info

Product

Resources

About