INTRINSIC ELLIPTICITY CORRELATION OF SDSS LUMINOUS RED GALAXIES AND MISALIGNMENT WITH THEIR HOST DARK MATTER HALOS

ABSTRACT We introduce the LEnSed laeS in the Eboss suRvey (LESSER) project, which aims to search for lensed Lyman-α emitters (LAEs) in the Extended Baryon Oscillation Spectroscopic Survey (eBOSS). The final catalogue contains 361 candidate lensing systems. The lens galaxies are luminous red galaxies (LRGs) at redshift 0.4 < z < 0.8, and the source galaxies are LAEs at redshift 2 < z < 3. The spectral resolution of eBOSS (∼2000) allows us to further identify the fine structures of Lyman-α ($\rm Ly\alpha$) emissions. Among our lensed LAE candidates, 281 systems present single-peaked line profiles while 80 systems show double-peaked features. Future spectroscopic/imaging follow-up observations of the catalogue may shed light on the origin of diverse $\rm Ly\alpha$ line morphology, and provide promising labs for studying low-mass dark matter haloes/subhaloes.

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Where are the Luminous Red Galaxies (LRGs)? Using correlation measurements and lensing to relate LRGs to dark matter haloes

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stt1446 ◽

2013 ◽

Vol 435 (3) ◽

pp. 2345-2370 ◽

Cited By ~ 42

Author(s):

Chiaki Hikage ◽

Rachel Mandelbaum ◽

Masahiro Takada ◽

David N. Spergel

Keyword(s):

Dark Matter ◽

Luminous Red Galaxies ◽

Red Galaxies

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The Slow Growth of Massive Galaxies in Rapidly Growing Dark Matter Halos

Proceedings of the International Astronomical Union ◽

10.1017/s1743921310002851 ◽

2009 ◽

Vol 5 (S262) ◽

pp. 244-247

Author(s):

Michael J. I. Brown ◽

Keyword(s):

Dark Matter ◽

Rapid Growth ◽

Observational Studies ◽

Cold Dark Matter ◽

Slow Growth ◽

Stellar Mass ◽

Dark Matter Halos ◽

Massive Galaxies ◽

Stellar Masses ◽

Red Galaxies

AbstractIn cold dark matter cosmologies, the most massive dark matter halos are predicted to undergo rapid growth at z < 1. While there is the expectation that massive galaxies will also rapidly grow via merging, recent observational studies conclude that the stellar masses of the most massive galaxies grow by just ~ 30% at z < 1. We have used the observed space density and clustering of z < 1 red galaxies in Boötes to determine how these galaxies populate dark matter halos. In the most massive dark matter halos, central galaxy stellar mass is proportional to halo mass to the power of a ~1/3 and much of the stellar mass resides within satellite galaxies. As a consequence, the most massive galaxies grow slowly even though they reside within rapidly growing dark matter halos.

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Red Galaxies Growing in Dark Matter Halos

Proceedings of the International Astronomical Union ◽

10.1017/s1743921310008409 ◽

2009 ◽

Vol 5 (H15) ◽

pp. 87-87

Author(s):

Michael J. I. Brown ◽

Keyword(s):

Dark Matter ◽

Luminosity Function ◽

Slow Growth ◽

Stellar Mass ◽

Dark Matter Halos ◽

Massive Galaxies ◽

Central Galaxy ◽

Satellite Galaxies ◽

Massive Halos ◽

Red Galaxies

AbstractTo understand the slow growth of massive galaxies at z < 1, we have modeled how these galaxies populate dark matter halos. The models are constrained with the observed luminosity function and clustering of z < 1 red galaxies. In the most massive halos, much of the stellar mass resides within multiple satellite galaxies rather than a single central galaxy. Consequently, massive galaxies grow slowly within rapidly growing dark matter halos.

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Constraints on the Clumpiness of Dark Matter Halos Through Heating of Disk Galaxies

EAS Publications Series ◽

10.1051/eas:2003136 ◽

2003 ◽

Vol 10 ◽

pp. 95-95

Author(s):

E. Ardi ◽

T. Tsuchiya ◽

A. Burkert

Keyword(s):

Dark Matter ◽

Disk Galaxies ◽

Dark Matter Halos

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Constrained Simulations of Dark Matter Halos

EAS Publications Series ◽

10.1051/eas:2006038 ◽

2006 ◽

Vol 20 ◽

pp. 15-18

Author(s):

Y. Hoffman ◽

E. Romano-Díaz ◽

A. Faltenbacher ◽

D. Jones ◽

C. Heller ◽

...

Keyword(s):

Dark Matter ◽

Dark Matter Halos

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Modeling dark matter halos with nonlinear field theories

Physical Review D ◽

10.1103/physrevd.103.103519 ◽

2021 ◽

Vol 103 (10) ◽

Author(s):

R. A. C. Correa ◽

P. H. R. S. Moraes ◽

A. de Souza Dutra ◽

O. L. Dors ◽

W. de Paula ◽

...

Keyword(s):

Dark Matter ◽

Field Theories ◽

Dark Matter Halos ◽

Nonlinear Field

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On the formation and stability of fermionic dark matter halos in a cosmological framework

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3986 ◽

2020 ◽

Author(s):

Carlos R Argüelles ◽

Manuel I Díaz ◽

Andreas Krut ◽

Rafael Yunis

Keyword(s):

Black Hole ◽

Dark Matter ◽

Space Distribution ◽

Coarse Grained ◽

Dark Matter Halos ◽

The Core ◽

The Galaxy ◽

Gravitating Systems ◽

The Given ◽

First Time

Abstract The formation and stability of collisionless self-gravitating systems is a long standing problem, which dates back to the work of D. Lynden-Bell on violent relaxation, and extends to the issue of virialization of dark matter (DM) halos. An important prediction of such a relaxation process is that spherical equilibrium states can be described by a Fermi-Dirac phase-space distribution, when the extremization of a coarse-grained entropy is reached. In the case of DM fermions, the most general solution develops a degenerate compact core surrounded by a diluted halo. As shown recently, the latter is able to explain the galaxy rotation curves while the DM core can mimic the central black hole. A yet open problem is whether this kind of astrophysical core-halo configurations can form at all, and if they remain stable within cosmological timescales. We assess these issues by performing a thermodynamic stability analysis in the microcanonical ensemble for solutions with given particle number at halo virialization in a cosmological framework. For the first time we demonstrate that the above core-halo DM profiles are stable (i.e. maxima of entropy) and extremely long lived. We find the existence of a critical point at the onset of instability of the core-halo solutions, where the fermion-core collapses towards a supermassive black hole. For particle masses in the keV range, the core-collapse can only occur for Mvir ≳ E9M⊙ starting at zvir ≈ 10 in the given cosmological framework. Our results prove that DM halos with a core-halo morphology are a very plausible outcome within nonlinear stages of structure formation.

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Clustering dependence of Chandra COSMOS Legacy AGN on host galaxy properties

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320002987 ◽

2019 ◽

Vol 15 (S356) ◽

pp. 226-226

Author(s):

Viola Allevato

Keyword(s):

Dark Matter ◽

Formation Rate ◽

Stellar Mass ◽

Active Galaxies ◽

Host Galaxy ◽

Mass Star ◽

Mass Relation ◽

Dark Matter Halos ◽

X Ray

AbstractThe presence of a super massive BH in almost all galaxies in the Universe is an accepted paradigm in astronomy. How these BHs form and how they co-evolve with the host galaxy is one of the most intriguing unanswered problems in modern Cosmology and of extreme relevance to understand the issue of galaxy formation. Clustering measurements can powerfully test theoretical model predictions of BH triggering scenarios and put constraints on the typical environment where AGN live in, through the connection with their host dark matter halos. In this talk, I will present some recent results on the AGN clustering dependence on host galaxy properties, such as galaxy stellar mass, star formation rate and specific BH accretion rate, based on X-ray selected Chandra COSMOS Legacy Type 2 AGN. We found no significant AGN clustering dependence on galaxy stellar mass and specif BHAR for Type 2 COSMOS AGN at mean z ∼ 1.1, with a stellar - halo mass relation flatter than predicted for non active galaxies in the Mstar range probed by our sample. We also observed a negative clustering dependence on SFR, with AGN hosting halo mass increasing with decreasing SFR. Mock catalogs of active galaxies in hosting dark matter halos with logMh[Msun] > 12.5, matched to have the same X-ray luminosity, stellar mass and BHAR of COSMOS AGN predict the observed Mstar - Mh, BHAR - Mh and SFR-Mh relations, at z ∼ 1.

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