Quasi-stellar objects and galaxy mass density profiles derived using the submillimetre galaxies magnification bias

被引：5

作者：

Crespo, D. ^{[1
,2
]}

Gonzalez-Nuevo, J. ^{[1
,2
]}

Bonavera, L. ^{[1
,2
]}

Cueli, M. M. ^{[1
,2
]}

Casas, J. M. ^{[1
,2
]}

Goitia, E. ^{[1
]}

机构：

[1] Univ Oviedo, Dept Fis, C Federico Garcia Lorca 18, Oviedo 33007, Spain

[2] Inst Univ Ciencias & Tecnol Espaciales Asturias, C Independencia 13, Oviedo 33004, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2022年 / 667卷

关键词：

galaxies: clusters: general; galaxies: high-redshift; submillimeter: galaxies; gravitational lensing: weak; dark matter; DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; LUMINOUS RED GALAXIES; DATA RELEASE; HERSCHEL-ATLAS; ASSEMBLY GAMA; COSMIC MAGNIFICATION; STAR-FORMATION; LENS SEARCH; CLUSTERS;

D O I：

10.1051/0004-6361/202244016

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The magnification bias on the submillimetre galaxies (SMGs) is a gravitational lensing e ffect, where the SMGs are used as background lensed galaxies. This e ffect can be used to investigate the mass density profiles of di fferent types of foreground lenses. Aims. In this work, we want to exploit the magnification bias of the SMGs using two di fferent foreground samples, quasi-stellar objects (QSOs) and galaxies. Our aim is to study and compare their mass density profiles and estimate their masses and concentrations. Methods. The background SMG sample consists of objects observed by Herschel with 1:2 < z < 4:0 (mean redshift at similar to 2:2). The foreground samples are QSOs with spectroscopic redshifts 0:2 < z < 1:0 (mean redshift at similar to 0:7) and massive galaxies with also spectroscopic redshifts 0:2 < z < 1:0 (mean redshift at similar to 0:3). The cross-correlation measurements are estimated with the DavisPeebles estimator by stacking the SMG-QSO and SMG-galaxy pairs for the two analysed cases, respectively. The advantage of such an approach is that it allows us to study the mass density profile over a wide range of angular scales, from similar to 2 to similar to 250 arcsec, including the inner part of the dark-matter halo (less than or similar to 100 kpc). Moreover, the analysis is carried out by combining two of the most common theoretical mass density profiles in order to fit the cross-correlation measurements. Results. The measurements are correctly fitted after splitting the available angular scales into an inner and an outer part using two independent mass density profiles, one for each region. In particular, for the QSOs, we obtain masses of log(10)(M/M-circle dot ) = 13:51 +/- 0:04 and of log(10)( M/M-circle dot) = 13:44 +/- 0:17 for the inner and outer parts, respectively. The estimated masses for the galaxy sample are log(10)( M/M-circle dot) = 13:32 +/- 0:08 and log(10)(M/M-circle dot) = 12:78 +/- 0:21 for the inner and outer parts, respectively. The concentrations for the inner part are much higher than those for the outer region for both samples: C = 6:85 +/- 0:34 (inner) and C = 0:36 +/- 0:18 (outer) for the QSOs and C = 8:23 +/- 0:77 (inner) and C = 1:21 +/- 1:01 (outer) for the galaxies. Conclusions. In both samples, the inner part has an excess in the mass density profile with respect to the outer part for both QSOs and galaxy samples. We obtain similar values for the central mass with both samples, and they are also in agreement with those of galaxy clusters results. However, the estimated masses for the outer region and the concentrations of the inner region both vary with lens sample. We believe this to be related to the probability of galactic interactions and /or the di fferent evolutionary stages.

引用

页数：11

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