Stellar Mass Loss in Elliptical Galaxies and the Fueling of Active Galactic Nuclei

AbstractThe formation of the brightest cluster galaxies (BCG) is a challenge for galaxy formation theory. We performed high resolution cosmological hydrodynamical simulations with the AMR code RAMSES to study the properties of the BCG which forms at the center of a Virgo–like cluster. We compare the results of 2 galaxy formation scenarios, one in which only supernovae feedback is included, and one in which also AGN feedback is considered. Properties of the simulated BCG which are comparable with those of observed massive elliptical galaxies and BCGs cannot be obtained if AGN feedback is not considered. The stellar-to-halo mass ratio in simulations without AGN feedback appears too large when compared to observations, while it is compatible the observationally determined values when AGN feedback is included. The kinematical and structural properties of the BCG are extremely different in the two models. When we do not include AGN feedback, the BCG is quickly rotating, with high Sérsic index, a clear mass excess in the center and a very large stellar mass fraction. When AGN feedback is considered, the BCG is slowly rotating, with a significantly cored surface density profile and low stellar mass fraction.

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The co-responsibility of mass and environment in the formation of lenticular galaxies

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320001908 ◽

2020 ◽

Vol 15 (S359) ◽

pp. 173-174

Author(s):

A. Cortesi ◽

L. Coccato ◽

M. L. Buzzo ◽

K. Menéndez-Delmestre ◽

T. Goncalves ◽

...

Keyword(s):

Active Galactic Nuclei ◽

Maximum Likelihood Method ◽

Spiral Galaxies ◽

Galactic Nuclei ◽

Rotation Velocity ◽

Elliptical Galaxies ◽

Likelihood Method ◽

Data Set ◽

Lenticular Galaxies ◽

Galaxies Kinematics

AbstractWe present the latest data release of the Planetary Nebulae Spectrograph Survey (PNS) of ten lenticular galaxies and two spiral galaxies. With this data set we are able to recover the galaxies’ kinematics out to several effective radii. We use a maximum likelihood method to decompose the disk and spheroid kinematics and we compare it with the kinematics of spiral and elliptical galaxies. We build the Tully- Fisher (TF) relation for these galaxies and we compare with data from the literature and simulations. We find that the disks of lenticular galaxies are hotter than the disks of spiral galaxies at low redshifts, but still dominated by rotation velocity. The mechanism responsible for the formation of these lenticular galaxies is neither major mergers, nor a gentle quenching driven by stripping or Active Galactic Nuclei (AGN) feedback.

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Excitation mechanism in the intracluster filaments surrounding the Brightest Cluster Galaxies

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320002343 ◽

2019 ◽

Vol 15 (S359) ◽

pp. 185-187

Author(s):

Fiorella L. Polles

Keyword(s):

Active Galactic Nuclei ◽

Galactic Nuclei ◽

Elliptical Galaxies ◽

Cluster Galaxies ◽

Cooling Flow ◽

Submillimeter Wavelengths ◽

Hot Plasma ◽

Brightest Cluster Galaxies ◽

Multi Phase ◽

The Impact

AbstractMulti-phase filamentary structures surrounding giant elliptical galaxies at the center of cool-core clusters, the Brightest Cluster Galaxies (BCGs), have been detected from optical to submillimeter wavelengths. The source of the ionisation in the filaments is still debated. Studying the excitation of these structures is key to our understanding of Active Galactic Nuclei (AGN) feedback in general, and more precisely of the impact of environmental and local effects on star formation. One possible contributor to the excitation of the filaments is the thermal radiation from the cooling of the hot plasma surrounding the BCGs, the so-called cooling flow.

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Chandra COSMOS Legacy Survey: Clustering dependence of Type 2 active galactic nuclei on host galaxy properties

Astronomy and Astrophysics ◽

10.1051/0004-6361/201936191 ◽

2019 ◽

Vol 632 ◽

pp. A88

Author(s):

V. Allevato ◽

A. Viitanen ◽

A. Finoguenov ◽

F. Civano ◽

H. Suh ◽

...

Keyword(s):

Active Galactic Nuclei ◽

Large Scale ◽

Formation Rate ◽

Galactic Nuclei ◽

Stellar Mass ◽

Host Galaxy ◽

X Ray ◽

Normal Galaxies ◽

Massive Halos

Aims. We perform clustering measurements of 800 X-ray selected Chandra COSMOS Legacy (CCL) Type 2 active galactic nuclei (AGN) with known spectroscopic redshift to probe the halo mass dependence on AGN host galaxy properties, such as galaxy stellar mass Mstar, star formation rate (SFR), and specific black hole accretion rate (BHAR; λBHAR) in the redshift range z = [0−3]. Methods. We split the sample of AGN with known spectroscopic redshits according to Mstar, SFR and λBHAR, while matching the distributions in terms of the other parameters, including redshift. We measured the projected two-point correlation function wp(rp) and modeled the clustering signal, for the different subsamples, with the two-halo term to derive the large-scale bias b and corresponding typical mass of the hosting halo. Results. We find no significant dependence of the large-scale bias and typical halo mass on galaxy stellar mass and specific BHAR for CCL Type 2 AGN at mean z ∼ 1, while a negative dependence on SFR is observed, i.e. lower SFR AGN reside in richer environment. Mock catalogs of AGN, matched to have the same X-ray luminosity, stellar mass, λBHAR, and SFR of CCL Type 2 AGN, almost reproduce the observed Mstar − Mh, λBHAR − Mh and SFR–Mh relations, when assuming a fraction of satellite AGN fAGNsat ∼ 0.15. This corresponds to a ratio of the probabilities of satellite to central AGN of being active Q ∼ 2. Mock matched normal galaxies follow a slightly steeper Mstar − Mh relation, in which low mass mock galaxies reside in less massive halos than mock AGN of similar mass. Moreover, matched mock normal galaxies are less biased than mock AGN with similar specific BHAR and SFR, at least for Q > 1.

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X-Ray Observations of Elliptical Galaxies by ASCA Satellite

Symposium - International Astronomical Union ◽

10.1017/s0074180900233317 ◽

1996 ◽

Vol 171 ◽

pp. 412-412

Author(s):

K. Matsushita ◽

K. Makishima

Keyword(s):

Low Temperature ◽

Mass Loss ◽

Elliptical Galaxies ◽

Stellar Mass ◽

Plasma Emission ◽

X Ray ◽

Theoretical Predictions ◽

Long Time ◽

Temperature Component ◽

Hubble Time

Using ASCA, we have confirmed that the ISM of X-ray bright elliptical galaxies are surprisingly metal poor, as compared to the theoretical predictions. In fact the exact values of the derived metallicity depend considerably on the plasma emission codes. However, the overall metallicity cannot be larger than ∼ 1 solar. For low LX/LB galaxies, all the available plasma codes suggest abundances less than half a solar. The ASCA spectra may be compatible with somewhat higher metallicity if we assume there is an additional low-temperature component (e.g. kTe ∼ 0.3 keV). However, the derived abundance can not be over 1 solar. In particular, the Si abundance turns out to be < 1.5 solar, confirming the metal-poor nature of the ISM. These ASCA results are in severe contradiction with most of the SN Ia rate, particularly that of Tammann (1982). Considering further that a fairly long time (109–10yr) is needed for the stellar mass loss to accumulates into the ISM, it is suggested that the SN Ia rate has remained quite low throughout Hubble time.

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Line-driven disc wind in near-Eddington active galactic nuclei: decrease of mass accretion rate due to powerful outflow

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa948 ◽

2020 ◽

Vol 494 (3) ◽

pp. 3616-3626 ◽

Cited By ~ 2

Author(s):

Mariko Nomura ◽

Ken Ohsuga ◽

Chris Done

Keyword(s):

Black Holes ◽

Mass Loss ◽

Active Galactic Nuclei ◽

Accretion Rate ◽

Galactic Nuclei ◽

Host Galaxy ◽

Radiation Hydrodynamics ◽

Iterative Technique ◽

X Ray ◽

Mass Accretion Rate

ABSTRACT Based on recent X-ray observations, ultrafast outflows from supermassive black holes are expected to have enough energy to dramatically affect their host galaxy but their launch and acceleration mechanisms are not well understood. We perform two-dimensional radiation hydrodynamics simulations of UV line-driven disc winds in order to calculate the mass-loss rates and kinetic power in these models. We develop a new iterative technique that reduces the mass accretion rate through the inner disc in response to the wind mass-loss. This makes the inner disc less UV bright, reducing the wind power compared to previous simulations which assumed a constant accretion rate with radius. The line-driven winds in our simulations are still extremely powerful, with around half the supplied mass accretion rate being ejected in the wind for black holes with mass 108–$10^{10}\, \mathrm{ M}_\odot$ accreting at L/LEdd = 0.5–0.9. Our results open up the way for estimating the growth rate of supermassive black hole and evaluating the kinetic energy ejected into the interstellar medium (active galactic nuclei feedback) based on a physical model of line-driven disc winds.

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On the fate of stellar mass loss in galactic nuclei

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/191.2.195 ◽

1980 ◽

Vol 191 (2) ◽

pp. 195-206 ◽

Cited By ~ 26

Author(s):

M. E. Bailey

Keyword(s):

Mass Loss ◽

Galactic Nuclei ◽

Stellar Mass

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Spin Evolution of Stellar-mass Black Hole Binaries in Active Galactic Nuclei

The Astrophysical Journal ◽

10.3847/1538-4357/aba2cc ◽

2020 ◽

Vol 899 (1) ◽

pp. 26 ◽

Cited By ~ 3

Author(s):

Hiromichi Tagawa ◽

Zoltán Haiman ◽

Imre Bartos ◽

Bence Kocsis

Keyword(s):

Black Hole ◽

Active Galactic Nuclei ◽

Galactic Nuclei ◽

Stellar Mass ◽

Black Hole Binaries ◽

Spin Evolution

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The dependence of mass and environment on the secular processes of AGNs in terms of morphology, colour, and specific star-formation rate

Astronomy and Astrophysics ◽

10.1051/0004-6361/201833328 ◽

2018 ◽

Vol 620 ◽

pp. A113 ◽

Cited By ~ 9

Author(s):

M. Argudo-Fernández ◽

I. Lacerna ◽

S. Duarte Puertas

Keyword(s):

Star Formation ◽

Active Galactic Nuclei ◽

Star Formation Rate ◽

Formation Rate ◽

Galactic Nuclei ◽

Stellar Mass ◽

High Mass ◽

Late Type ◽

Star Forming ◽

Isolated Galaxies

Context. Galaxy mass and environment play a major role in the evolution of galaxies. In the transition from star-forming to quenched galaxies, active galactic nuclei (AGNs) also have a principal action therein. However, the connections between these three actors are still uncertain. Aims. In this work we investigate the effects of stellar mass and the large-scale structure (LSS) environment on the fraction of optical nuclear activity in a population of isolated galaxies, where AGN would not be triggered by recent galaxy interactions or mergers. Methods. As a continuation of a previous work, we focus on isolated galaxies to study the effect of stellar mass and the LSS in terms of morphology (early- and late-type), colour (red and blue), and specific star-formation rate (quenched and star-forming). To explore where AGN activity is affected by the LSS, we separate galaxies into two groups, of low- and high mass, respectively, and use the tidal strength parameter to quantify the effects. Results. We found that AGN is strongly affected by stellar mass in “active” galaxies (namely late-type, blue, and star-forming), but that mass has no influence on “quiescent” galaxies (namely early-type, red, and quenched), at least for masses down to 1010 M⊙. In relation to the LSS, we found an increase in the fraction of star-forming nuclei galaxies with denser LSS in low-mass star-forming and red isolated galaxies. Regarding AGN, we find a clear increase in the fraction of AGNs with denser environment in quenched and red isolated galaxies, independently of the stellar mass. Conclusions. Active galactic nuclei activity appears to be “mass triggered” in active isolated galaxies. This means that AGN activity is independent of the intrinsic properties of the galaxies, but is dependent on their stellar mass. On the other hand, AGN activity appears to be “environment triggered” in quiescent isolated galaxies, where the fraction of AGNs as a function of specific star formation rate and colour increases from void regions to denser LSS, independently of stellar mass.

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