2014A&A...571A..65V


Query : 2014A&A...571A..65V

2014A&A...571A..65V - Astronomy and Astrophysics, volume 571A, 65-65 (2014/11-1)

Characterizing SL2S galaxy groups using the Einstein radius.

VERDUGO T., MOTTA V., FOEX G., FORERO-ROMERO J.E., MUNOZ R.P., PELLO R., LIMOUSIN M., MORE A., CABANAC R., SOUCAIL G., BLAKESLEE J.P., MEJIA-NARVAEZ A.J., MAGRIS G. and FERNANDEZ-TRINCADO J.G.

Abstract (from CDS):

We aim to study the reliability of RA (the distance from the arcs to the center of the lens) as a measure of the Einstein radius in galaxy groups. In addition, we want to analyze the possibility of using RA as a proxy to characterize some properties of galaxy groups, such as luminosity (L) and richness (N). We analyzed the Einstein radius, θE, in our sample of Strong Lensing Legacy Survey (SL2S) galaxy groups, and compared it with RA, using three different approaches: 1) the velocity dispersion obtained from weak lensing assuming a singular isothermal sphere profile (θE,I); 2) a strong lensing analytical method (θE,II) combined with a velocity dispersion-concentration relation derived from numerical simulations designed to mimic our group sample; and 3) strong lensing modeling (θE,III) of eleven groups (with four new models presented in this work) using Hubble Space Telescope (HST) and Canada-France-Hawaii Telescope (CFHT) images. Finally, RA was analyzed as a function of redshift z to investigate possible correlations with L, N, and the richness-to-luminosity ratio (N/L). We found a correlation between θE and RA, but with large scatter. We estimate θE,I=(2.2±0.9)+(0.7±0.2)RA, θE,II=(0.4±1.5)+(1.1±0.4)RA, and θE,III=(0.4±1.5)+(0.9±0.3)RA for each method respectively. We found weak evidence of anti-correlation between RA and z, with Log RA = (0.58 ±0.06) - (0.04 ±0.1)z, suggesting a possible evolution of the Einstein radius with z, as reported previously by other authors. Our results also show that RA is correlated with L and N (more luminous and richer groups have greater RA), and a possible correlation between RA and the N/L ratio. Our analysis indicates that RA is correlated with θE in our sample, making RA useful for characterizing properties like L and N (and possibly N/L) in galaxy groups. Additionally, we present evidence suggesting that the Einstein radius evolves with z.

Abstract Copyright:

Journal keyword(s): gravitational lensing: strong - galaxies: groups: general

Simbad objects: 23

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Number of rows : 23
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 [LCG2009] SL2S Group J02140-0532 GrG 02 14 08.0316 -05 35 32.621           ~ 7 0
2 [MCM2012] SA22 gLS 02 14 08.1 -05 35 32           ~ 4 0
3 [MCM2012] SA23 gLS 02 14 11.2 -04 05 03           ~ 3 0
4 [MCM2012] SA33 gLS 02 18 07.3 -05 15 36           ~ 3 0
5 [LCG2009] SL2S Group J02215-0647 GrG 02 21 51.183 -06 47 32.79           ~ 4 0
6 [MCM2012] SA39 gLS 02 21 51.2 -06 47 33           ~ 5 0
7 [MCM2012] SA50 gLS 02 25 46.1 -07 37 39           ~ 4 0
8 [LCG2009] SL2S Group J02254-0737 GrG 02 25 46.1184 -07 37 38.468           ~ 3 0
9 [MCM2012] SA63 gLS 08 52 07.2 -03 43 16           ~ 4 0
10 [MCM2012] SA66 gLS 08 54 46.5 -01 21 37           ~ 4 0
11 [LCG2009] SL2S Group J08544-0121 GrG 08 54 46.5480 -01 21 37.262           ~ 8 0
12 [LCG2009] SL2S Group J08591-0345 GrG 08 59 14.4576 -03 45 14.478           ~ 3 0
13 [MCM2012] SA72 gLS 08 59 14.6 -03 45 15           ~ 4 0
14 [MCM2012] SA80 gLS 09 59 56.0 +02 19 02           ~ 4 0
15 [FKC2008] COSMOS 0211+1139 gLS 10 02 11.2 +02 11 39           ~ 7 0
16 [MCM2012] SA97 gLS 14 08 13.8 +54 29 08           ~ 3 0
17 [LCG2009] SL2S Group J14081+5429 GrG 14 08 13.939 +54 29 04.68           ~ 5 0
18 [LCG2009] SL2S Group J14300+5546 GrG 14 30 00.660 +55 46 47.87           ~ 7 0
19 [MCM2012] SA112 gLS 14 30 00.7 +55 46 48           ~ 4 0
20 [LCG2009] SL2S Group J22133+0048 GrG 22 13 31.85760 +00 48 36.0977           ~ 3 0
21 [MCM2012] SA123 gLS 22 13 31.9 +00 48 36           ~ 4 0
22 [MCM2012] SA127 gLS 22 21 43.7 -00 53 03           ~ 4 0
23 3XMM J222144.0-005306 GrG 22 21 43.74240 -00 53 02.5549           ~ 6 0

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2022.05.28-09:04:01

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