scholarly journals Radiative feedback and cosmic molecular gas: the role of different radiative sources

2016 ◽  
Vol 460 (4) ◽  
pp. 3733-3752 ◽  
Author(s):  
Umberto Maio ◽  
Margarita Petkova ◽  
Gabriella De Lucia ◽  
Stefano Borgani
Keyword(s):  
Molecular Gas ◽  
Radiative Feedback

scholarly journals SMA observations of Haro 2: molecular gas around a hot superbubble

2020 ◽  
Vol 494 (1) ◽  
pp. 1-9
Author(s):  
Sara C Beck ◽  
Pei-Ying Hsieh ◽  
Jean Turner
Keyword(s):  
Dwarf Galaxy ◽  
Star Clusters ◽  
Molecular Gas ◽  
Apparent Velocity ◽  
Velocity Range ◽  
X Ray ◽  
Ideal Candidate ◽  
The Galaxy ◽  
Extended Emission

ABSTRACT Haro 2, a nearby dwarf starburst dwarf galaxy with strong Ly α emission, hosts a starburst that has created outflows and filaments. The clear evidence for galactic outflow makes it an ideal candidate for studying the role of molecular gas in feedback processes in a dwarf galaxy. We observed CO(2–1) in Haro 2 at the Submillimeter Array in the compact and extended configurations, and have mapped the molecular emission with velocity resolution 4.1 km s−1 and spatial resolution 2.0 × 1.6 arcsec2. With this significant increase of resolution over previous measurements, we see that the molecular gas comprises two components: bright clumps associated with the embedded star clusters of the starburst, and fainter extended emission east of the starburst region. The extended emission coincides with an X-ray bubble and has the kinematic signatures of an outflowing cone or of an expanding shell or bubble; the velocity range is ∼35 km s−1. We suggest that the starburst winds that created the X-ray bubble have entrained the molecular gas, and that the apparent velocity gradient at an angle to the photometric axis is an artefact caused by the outflow. The molecular and X-ray activity is on the east of the galaxy and the ionized outflow and optical filaments are west; their relationship is not clear.

scholarly journals Properties of the outer regions of spiral disks: abundances, colors and ages

2016 ◽  
Vol 11 (S321) ◽  
pp. 102-104
Author(s):  
Mercedes Mollá ◽  
Angeles I. Díaz ◽  
Brad K. Gibson ◽  
Oscar Cavichia ◽  
Ángel-R. López-Sánchez
Keyword(s):  
Star Formation ◽  
Chemical Evolution ◽  
Molecular Gas ◽  
Disk Galaxies ◽  
Gas Formation ◽  
Radial Profiles ◽  
Potential Origin

AbstractWe summarize the results obtained from our suite of chemical evolution models for spiral disks, computed for different total masses and star formation efficiencies. Once the gas, stars and star formation radial distributions are reproduced, we analyze the Oxygen abundances radial profiles for gas and stars, in addition to stellar averaged ages and global metallicity. We examine scenarios for the potential origin of the apparent flattening of abundance gradients in the outskirts of disk galaxies, in particular the role of molecular gas formation prescriptions.

scholarly journals The Role of Galactic Winds on Molecular Gas Emission from Galaxy Mergers

2008 ◽  
Vol 176 (2) ◽  
pp. 331-354 ◽  
Author(s):  
Desika Narayanan ◽  
Thomas J. Cox ◽  
Brandon Kelly ◽  
Romeel Davé ◽  
Lars Hernquist ◽  
...  
Keyword(s):  
Molecular Gas ◽  
Galaxy Mergers ◽  
Gas Emission ◽  
Galactic Winds

scholarly journals The molecular gas content in a protocluster at z = 17: Star formation and AGN feedback

2019 ◽  
Vol 15 (S352) ◽  
pp. 168-170
Author(s):  
Q. D’Amato ◽  
I. Prandoni ◽  
R. Gilli ◽  
M. Massardi ◽  
E. Liuzzo ◽  
...  
Keyword(s):  
Star Formation ◽  
Large Scale ◽  
Gas Content ◽  
Molecular Gas ◽  
Star Forming ◽  
Physical Conditions ◽  
Radio Jets ◽  
Multi Wavelength ◽  
Data Coverage

AbstractA large-scale structure has been recently discovered at z = 1.7, around a powerful FRII radio galaxy. Eight Star Forming Galaxies (SFGs) have been discovered within Δ z ≍ 0.0095 and at < 1 Mpc from the FRII, indicating that this is a signpost of a protocluster. Furthermore, a significant X-ray diffuse emission overlapping the Eastern lobe of the FRII has been detected. Protoclusters are the ideal targets to investigate the complex assembly processes leading to the formation of local galaxy clusters. We will exploit new ALMA CO(2-1) observations (PI: R. Gilli) of the entire region around the FRII galaxy to trace the molecular gas content, in order to discover new protocluster members. Coupling these measurements with the multi-wavelength data coverage available for this field, we aim at placing constrains on the physical conditions in which star formation occurs, and ultimately infer the role of the radio jets in triggering it.

The role of AGN in galaxy star formation: A case study of a radio galaxy at z = 2.6

2019 ◽  
Vol 15 (S356) ◽  
pp. 224-224
Author(s):  
Allison Man
Keyword(s):  
Star Formation ◽  
Radio Galaxy ◽  
Star Formation History ◽  
Molecular Gas ◽  
Ob Stars ◽  
Massive Galaxies ◽  
Radio Jets ◽  
Formation History

AbstractRadio galaxies are ideal sites to scrutinize AGN feedback physics, as they are massive galaxies with jets that interact with the surrounding ISM. I will present a detailed analysis of the recent star formation history and conditions of a starbursting, massive radio galaxy at z = 2.6, PKS 0529-549. In the 8.5-hour VLT/X-Shooter spectrum, we detect unambiguous signatures of stellar photospheric absorption lines originating from OB-stars. Comparison with model spectra shows that more than one burst took place in its recent past: the most recent one at 4 − 7 Myr, and another aged ⩾20 Myr. ALMA observations of the [CI] atomic carbon emission line indicates that it has a low molecular gas fraction (∼13%) and short depletion time (∼40 Myr). Most intriguing is the modest velocity dispersion (⩽50 km/s) of these photospheric lines and the ALMA [CI] cold gas. We attribute its efficient star formation to compressive gas motions, induced by radio jets and/or interaction. Star formation works in concert with the AGN to remove any residual molecular gas and eventually leads to quenching.

scholarly journals Molecular gas in the central region of NGC 7213

2020 ◽  
Vol 641 ◽  
pp. A151
Author(s):  
F. Salvestrini ◽  
C. Gruppioni ◽  
F. Pozzi ◽  
C. Vignali ◽  
A. Giannetti ◽  
...  
Keyword(s):  
Star Formation ◽  
Emission Line ◽  
Large Scale ◽  
Host Galaxy ◽  
Molecular Gas ◽  
X Ray ◽  
Gas Kinematics ◽  
Star Formation Activity ◽  
Multi Wavelength

We present a multi-wavelength study (from X-ray to mm) of the nearby low-luminosity active galactic nucleus NGC 7213. We combine the information from the different bands to characterise the source in terms of contribution from the AGN and the host-galaxy interstellar medium. This approach allows us to provide a coherent picture of the role of the AGN and its impact, if any, on the star formation and molecular gas properties of the host galaxy. We focused our study on archival ALMA Cycle 1 observations, where the CO(2–1) emission line has been used as a tracer of the molecular gas. Using the 3DBAROLO code on ALMA data, we performed the modelling of the molecular gas kinematics traced by the CO(2–1) emission, finding a rotationally dominated pattern. The molecular gas mass of the host galaxy was estimated from the integrated CO(2–1) emission line obtained with APEX data, assuming an αCO conversion factor. Had we used the ALMA data, we would have underestimated the gas masses by a factor ∼3, given the filtering out of the large-scale emission in interferometric observations. We also performed a complete X-ray spectral analysis on archival observations, revealing a relatively faint and unobscured AGN. The AGN proved to be too faint to significantly affect the properties of the host galaxy, such as star formation activity and molecular gas kinematics and distribution.

scholarly journals Dense Molecular Gas and the Role of Star Formation in the Host Galaxies of Quasi?stellar Objects

2006 ◽  
Vol 132 (6) ◽  
pp. 2398-2408 ◽  
Author(s):  
A. S. Evans ◽  
P. M. Solomon ◽  
L. J. Tacconi ◽  
T. Vavilkin ◽  
D. Downes
Keyword(s):  
Star Formation ◽  
Molecular Gas ◽  
Host Galaxies ◽  
Stellar Objects ◽  
Quasi Stellar Objects

scholarly journals 5.4. New high-resolution observations of molecular gas towards the center of spiral galaxies

1998 ◽  
Vol 184 ◽  
pp. 217-218
Author(s):  
S. Garcia-Burillo
Keyword(s):  
High Resolution ◽  
Spiral Galaxies ◽  
Specific Role ◽  
Molecular Gas ◽  
Gas Distribution ◽  
Limited Sample ◽  
Secular Evolution ◽  
Hubble Sequence

We discuss the major results from a study of the molecular gas distribution and dynamics in the nuclear disks (ND) of a limited sample of nearby spirals: NGC891, NGC5907, NGC4565, NGC4013, NGC4321, M82, NGC3626 and NGC3593. The main objective is to search for observational evidences of secular evolution along the Hubble sequence in spirals and to study the specific role of bars in the process.

scholarly journals Disk growth in bulge-dominated galaxies: molecular gas and morphological evolution

2007 ◽  
Vol 3 (S245) ◽  
pp. 173-176
Author(s):  
Lisa Young ◽  
Martin Bureau ◽  
Alison Crocker ◽  
Francoise Combes
Keyword(s):  
Morphological Evolution ◽  
Stellar Mass ◽  
Young Stars ◽  
Molecular Gas ◽  
Early Type ◽  
Future Studies ◽  
Lenticular Galaxies ◽  
Star Formation Activity ◽  
Disk Growth

AbstractSubstantial numbers of morphologically regular early-type (elliptical and lenticular) galaxies contain molecular gas, and the quantities of gas are probably sufficient to explain recent estimates of the current level of star formation activity. This gas can also be used as a tracer of the processes that drive the evolution of early-type galaxies. For example, in most cases the gas is forming dynamically cold stellar disks with sizes in the range of hundreds of pc to more than one kpc, although there is typically only 1% of the total stellar mass currently available to form young stars. The numbers are still small, but the molecular kinematics indicate that some of the gas probably originated from internal stellar mass loss while some was acquired from outside. Future studies will help to quantify the role of molecular gas (dissipational processes) in the formation of early-type galaxies and their evolution along the red sequence.

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