scholarly journals The Recent Evolution of Early-Type Galaxies as Seen in their Cold Gas

2014 ◽  
Vol 10 (S309) ◽  
pp. 47-52
Author(s):  
Lisa M. Young
Keyword(s):  
Star Formation History ◽  
Molecular Gas ◽  
Early Type ◽  
Stellar Kinematics ◽  
Ionized Gas ◽  
Gas Kinematics ◽  
Formation History ◽  
Galaxy Assembly ◽  
Early Type Galaxy ◽  
Cold Gas

AbstractI present an overview of new observations of atomic and molecular gas in early-type galaxies, focusing on the Atlas3D project. Our data on stellar kinematics, age and metallicity, and ionized gas kinematics allow us to place the cold gas into the broader context of early-type galaxy assembly and star formation history. The cold gas data also provide valuable constraints for numerical simulations of early-type galaxies.

scholarly journals Mapping the dark matter halo of early-type galaxy NGC 2974 through orbit-based models with combined stellar and cold gas kinematics

2019 ◽  
Vol 491 (3) ◽  
pp. 4221-4231 ◽  
Author(s):  
Meng Yang ◽  
Ling Zhu ◽  
Anne-Marie Weijmans ◽  
Glenn van de Ven ◽  
Nicholas Boardman ◽  
...  
Keyword(s):  
Dark Matter ◽  
Dark Matter Halo ◽  
Dark Halo ◽  
Confidence Limits ◽  
Early Type ◽  
Stellar Kinematics ◽  
Stellar Orbits ◽  
Gas Kinematics ◽  
Early Type Galaxy ◽  
Cold Gas

ABSTRACT We present an orbit-based method of combining stellar and cold gas kinematics to constrain the dark matter profile of early-type galaxies. We apply this method to early-type galaxy NGC 2974, using Pan-STARRS imaging and SAURON stellar kinematics to model the stellar orbits, and introducing H i kinematics from VLA observation as a tracer of the gravitational potential. The introduction of the cold gas kinematics shows a significant effect on the confidence limits of especially the dark halo properties: we exclude more than $95{{\ \rm per\ cent}}$ of models within the 1σ confidence level of Schwarzschild modelling with only stellar kinematics, and reduce the relative uncertainty of the dark matter fraction significantly to $10{{\ \rm per\ cent}}$ within 5Re. Adopting a generalized Navarro–Frenk–White (NFW) dark matter profile, we measure a shallow cuspy inner slope of $0.6^{+0.2}_{-0.3}$ when including the cold gas kinematics in our model. We cannot constrain the inner slope with the stellar kinematics alone.

scholarly journals 5.15. Star formation and molecular gas in NGC 404

1998 ◽  
Vol 184 ◽  
pp. 241-242 ◽  
Author(s):  
J. Cepa ◽  
B. Vila ◽  
N. Nakai ◽  
K. Kohno ◽  
R. Kawabe
Keyword(s):  
Star Formation ◽  
Elliptical Galaxies ◽  
Molecular Gas ◽  
Early Type ◽  
Ionized Gas ◽  
General Properties ◽  
Cool Gas ◽  
Cold Gas

The last decade has brought about a completely different picture of elliptical galaxies. The once considered completely inert systems have revealed the presence of fair amount of dust, cool and cold gas, and undergoing star formation. The current statistics is that 80% of elliptical galaxies have detectable cool gas components, and as many as 60% have ionized gas (Knapp et al. 1989, Goudfrooij et al. 1994). Several single-dish CO surveys have been reported in the literature, allowing the deduction of several general properties of the molecular gas in early-type galaxies (Sage & Wrobel 1989, Lees et al. 1991, Wiklind et al. 1995).

scholarly journals The Star Formation History of the Virgo Early‐Type Galaxy NGC 4435: TheSpitzerMid‐Infrared View

2007 ◽  
Vol 656 (1) ◽  
pp. 206-216 ◽  
Author(s):  
P. Panuzzo ◽  
O. Vega ◽  
A. Bressan ◽  
L. Buson ◽  
M. Clemens ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation History ◽  
Early Type ◽  
Formation History ◽  
History Of ◽  
Early Type Galaxy

Galactic dynamics and DM profile of NGC1380 with ALMA and VLT/MUSE

2019 ◽  
Vol 14 (S353) ◽  
pp. 248-252
Author(s):  
Takafumi Tsukui ◽  
Satoru Iguchi ◽  
Kyoko Onishi
Keyword(s):  
Dark Matter ◽  
Galaxy Evolution ◽  
Neutral Hydrogen ◽  
Hydrogen Gas ◽  
Large Field ◽  
Molecular Gas ◽  
Early Type ◽  
Stellar Kinematics ◽  
Gas Kinematics ◽  
The Galaxy

AbstractIn order to understand the interaction between dark matter and baryonic matter in the galaxy evolution history, it is fundamental to constrain dark matter (DM) distribution in galaxies. However, it is difficult to constrain DM profile in the central region of early type galaxy because of the lack of extended neutral hydrogen gas and the degeneracy between dynamical stellar M/L and DM profile. To resolve this difficulty, we conducted combined analysis of ALMA cold molecular gas kinematics and MUSE stellar kinematics of early type fast rotator galaxy NGC1380. In addition, we used HST image to trace the stellar luminosity distribution. With the help of high resolution of ALMA image and large field of view of MUSE, we derived the central BH mass, stellar bulge, disk and DM profile.

Unveiling the nuclear region of NGC 6868: Mapping the stellar population and ionized gas

2019 ◽  
Vol 15 (S359) ◽  
pp. 418-420
Author(s):  
João P. V. Benedetti ◽  
Rogério Riffel ◽  
Tiago V. Ricci ◽  
João E. Steiner ◽  
Rogemar A. Riffel ◽  
...  
Keyword(s):  
Stellar Population ◽  
Star Formation History ◽  
Nuclear Region ◽  
Stellar Kinematics ◽  
Ionized Gas ◽  
Formation History ◽  
The Galaxy ◽  
History Of ◽  
Field Unit ◽  
New Generation

AbstractWe mapped the stellar population and emission gas properties in the nuclear region of NGC 6868 using datacubes extracted with Gemini Multi-Object Spectrograph (GMOS) in the Integral Field Unit (IFU) mode. To obtain the star-formation history of this galaxy we used the starlight code together with the new generation of MILES simple stellar population models. The stellar population dominating (95% in light fraction) the central region of NGC 6868 is old and metal rich (~10 Gyr, 2.2 Z⊙). We also derived the kinematics and emission line fluxes of ionized gas with the IFSCube package. A rotation disk is clearly detected in the nuclear region of the galaxy and no broad components were detected. Also, there is a region where the emission lines disappear almost completely, probably due to diffuse ionized gas component. Channel maps, diagnostic diagrams and stellar kinematics are still under analysis.

scholarly journals Quenching by gas compression and consumption

2019 ◽  
Vol 624 ◽  
pp. A81 ◽  
Author(s):  
Allison W. S. Man ◽  
Matthew D. Lehnert ◽  
Joël D. R. Vernet ◽  
Carlos De Breuck ◽  
Theresa Falkendal
Keyword(s):  
Star Formation ◽  
Formation Rate ◽  
Relative Strength ◽  
Star Formation History ◽  
Molecular Gas ◽  
Host Galaxies ◽  
Massive Galaxies ◽  
Star Forming ◽  
Gas Compression ◽  
Formation History

The objective of this work is to study how active galactic nuclei (AGN) influence star formation in host galaxies. We present a detailed investigation of the star-formation history and conditions of a z = 2.57 massive radio galaxy based on VLT/X-shooter and ALMA observations. The deep rest-frame ultraviolet spectrum contains photospheric absorption lines and wind features indicating the presence of OB-type stars. The most significantly detected photospheric features are used to characterize the recent star formation: neither instantaneous nor continuous star-formation history is consistent with the relative strength of the Si IIλ1485 and S Vλ1502 absorption. Rather, at least two bursts of star formation took place in the recent past, at 6+1-2 Myr and ≳20 Myr ago, respectively. We deduce a molecular H2 gas mass of (3.9 ± 1.0) × 1010 M⊙ based on ALMA observations of the [C I] 3P2−3P1 emission. The molecular gas mass is only 13% of its stellar mass. Combined with its high star-formation rate of (1020-170+190 M⊙ yr-1, this implies a high star-formation efficiency of (26 ± 8) Gyr−1 and a short depletion time of (38 ± 12) Myr. We attribute the efficient star formation to compressive gas motions in order to explain the modest velocity dispersions (⩽55 km s−1) of the photospheric lines and of the star-forming gas traced by [C I]. Because of the likely very young age of the radio source, our findings suggest that vigorous star formation consumes much of the gas and works in concert with the AGN to remove any residual molecular gas, and eventually quenching star formation in massive galaxies.

scholarly journals The Structure and Star Formation History of Early‐Type Galaxies in the Ultra Deep Field/GRAPES Survey

2006 ◽  
Vol 636 (1) ◽  
pp. 115-133 ◽  
Author(s):  
A. Pasquali ◽  
I. Ferreras ◽  
N. Panagia ◽  
E. Daddi ◽  
S. Malhotra ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation History ◽  
Early Type ◽  
Formation History ◽  
History Of

scholarly journals Molecular and ionized gas kinematics in the GC Radio Arc

2016 ◽  
Vol 11 (S322) ◽  
pp. 133-136
Author(s):  
N. Butterfield ◽  
C.C. Lang ◽  
E. A. C. Mills ◽  
D. Ludovici ◽  
J. Ott ◽  
...  
Keyword(s):  
Star Formation ◽  
Molecular Cloud ◽  
Molecular Clouds ◽  
Radio Continuum ◽  
Molecular Gas ◽  
The South ◽  
Ionized Gas ◽  
Molecular Emission ◽  
Gas Kinematics

AbstractWe present NH3 and H64α+H63α VLA observations of the Radio Arc region, including the M0.20 – 0.033 and G0.10 – 0.08 molecular clouds. These observations suggest the two velocity components of M0.20 – 0.033 are physically connected in the south. Additional ATCA observations suggest this connection is due to an expanding shell in the molecular gas, with the centroid located near the Quintuplet cluster. The G0.10 – 0.08 molecular cloud has little radio continuum, strong molecular emission, and abundant CH3OH masers, similar to a nearby molecular cloud with no star formation: M0.25+0.01. These features detected in G0.10 – 0.08 suggest dense molecular gas with no signs of current star formation.

scholarly journals SuperMassive Blackholes grow from stellar BHs of star formation history?

2015 ◽  
Vol 11 (S319) ◽  
pp. 64-65
Author(s):  
Brigitte Rocca-Volmerange
Keyword(s):  
Black Hole ◽  
Star Formation ◽  
Star Formation History ◽  
Spectral Energy ◽  
Energy Distributions ◽  
Formation History ◽  
The Galaxy ◽  
Black Hole Masses ◽  
Early Type Galaxy ◽  
Size Scales

AbstractThe origin of the supermassive black hole masses MSMBH discovered at the highest redshifts is still actively debated. Moreover the statistically significant relation of MSMBH with bulge luminosities LV, extended on several magnitude orders, confirms a common physical process linking small (≤ 1pc) to large (kpcs) size scales. The Spectral Energy Distributions (SEDs) of two z=3.8 radio galaxies 4C41.17 and TN J2007-1316, best-fitted by evolved early type galaxy and starburst scenarios also imply masses of stellar remnants. Computed with the evolutionary code Pegase.3, the cumulated stellar black hole mass MsBH reach up to several 109M⊙, similar to MSMBH at same z. We propose the SMBH growth is due to the migration of the stellar dense residues (sBH) towards the galaxy core by dynamical friction. Discussed in terms of time-scales, this process which is linking AGN and star formation, also fully justifies the famous relation MSMBH-LV.

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