Molecular Gas and Star Formation in Nearby Galaxies

2008 ◽  
pp. 231-236
Author(s):  
Shinya Komugi ◽  
Yoshiaki Sofue ◽  
Hiroyuki Nakanishi ◽  
Sachiko Onodera ◽  
Fumi Egusa ◽  
...  
Keyword(s):  
Star Formation ◽  
Molecular Gas ◽  
Nearby Galaxies

scholarly journals SKA studies of nearby galaxies: star-formation, accretion processes and molecular gas across all environments

2015 ◽  
Author(s):  
Rob J. Beswick ◽  
Elias Brinks ◽  
Miguel Perez-Torres ◽  
Anita Richards ◽  
Susanne Aalto ◽  
...  
Keyword(s):  
Star Formation ◽  
Molecular Gas ◽  
Nearby Galaxies

scholarly journals High-J CO Intensity Measurements for Galaxies Observed by the Herschel FTS

2015 ◽  
Vol 11 (S315) ◽  
pp. 26-29
Author(s):  
Julia Kamenetzky ◽  
Naseem Rangwala ◽  
Jason Glenn ◽  
Philip Maloney ◽  
Alex Conley
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Raw Material ◽  
Molecular Gas ◽  
Star Forming ◽  
Star Forming Regions ◽  
J 13 ◽  
Systematic Effects ◽  
Nearby Galaxies ◽  
Co Emission

AbstractMolecular gas is the raw material for star formation and is commonly traced by the carbon monoxide (CO) molecule. The atmosphere blocks all but the lowest-J transitions of CO for observatories on the ground, but the launch of the Herschel Space Observatory revealed the CO emission of nearby galaxies from J = 4−3 to J = 13−12. Herschel showed that mid- and high-J CO lines in nearby galaxies are emitted from warm gas, accounting for approximately 10% of the molecular mass, but the majority of the CO luminosity. The energy budget of this warm, highly-excited gas is a significant window into the feedback interactions among molecular gas, star formation, and galaxy evolution. Likely, mechanical heating is required to explain the excitation. Such gas has also been observed in star forming regions within our galaxy.We have examined all ~300 spectra of galaxies from the Herschel Fourier Transform Spectrometer and measured line fluxes or upper limits for the CO J = 4−3 to J = 13−12, [CI], and [NII] 205 micron lines in ~200 galaxies, taking systematic effects of the FTS into account. We will present our line fitting method, illustrate trends available so far in this large sample, and preview the full 2-component radiative transfer likelihood modeling of the CO emission using an illustrative sample of 20 galaxies, including comparisons to well-resolved galactic regions. This work is a comprehensive study of mid- and high-J CO emission among a variety of galaxy types, and can be used as a resource for future (sub)millimeter studies of galaxies with ground-based instruments.

scholarly journals Molecular Gas and Star Formation in BIMA SONG Bars

2001 ◽  
Vol 205 ◽  
pp. 348-349
Author(s):  
Kartik Sheth ◽  
S.N. Vogel ◽  
A.I. Harris ◽  
M.W. Regan ◽  
M.D. Thornley ◽  
...  
Keyword(s):  
Star Formation ◽  
Massive Star ◽  
Molecular Gas ◽  
Gas Flows ◽  
Gas Distribution ◽  
Hydrodynamic Models ◽  
Massive Star Formation ◽  
Downstream Side ◽  
Star Formation Activity ◽  
Nearby Galaxies

Using a sample of 7 barred spirals from the BIMA Survey of Nearby Galaxies (SONG), we compare the molecular gas distribution in the bar, to recent massive star formation activity. In all 7 galaxies, Hα is offset azimuthally from the CO on the downstream side. The maximum offset, at the bar ends, ranges from 170-570 pc, with an average of 320±120 pc. We discuss whether the observed offsets are consistent with the description of gas flows in bars provided by the two main classes of models: n-body models and hydrodynamic models.

scholarly journals Molecular gas in galaxies: changing conditions from disks to starbursts

2015 ◽  
Vol 11 (S315) ◽  
pp. 199-206
Author(s):  
Christine D. Wilson
Keyword(s):  
Star Formation ◽  
Interstellar Medium ◽  
Galaxy Evolution ◽  
Surface Density ◽  
Physical State ◽  
Active Galaxies ◽  
Molecular Gas ◽  
Central Question ◽  
Space Observatory ◽  
Nearby Galaxies

AbstractIn understanding galaxy evolution, one central question is how star formation is regulated in galaxies. Changes in star formation rates are likely tied to changes in the interstellar medium, particularly the molecular gas which is the fuel for star formation. I will discuss our recent results which use data from the Herschel Space Observatory, the Atacama Large Millimeter/submillimeter Array, and other telescopes to determine the typical density, temperature, and surface density of the molecular gas in various nearby galaxies. Comparing the properties of molecular gas in starburst and other active galaxies with more quiescent spiral disks provides some clues as to how changes in the physical state of the gas, such as mean density, can lead to enhanced star formation rates.

scholarly journals CARMA SURVEY TOWARD INFRARED-BRIGHT NEARBY GALAXIES (STING). II. MOLECULAR GAS STAR FORMATION LAW AND DEPLETION TIME ACROSS THE BLUE SEQUENCE

2012 ◽  
Vol 745 (2) ◽  
pp. 183 ◽  
Author(s):  
Nurur Rahman ◽  
Alberto D. Bolatto ◽  
Rui Xue ◽  
Tony Wong ◽  
Adam K. Leroy ◽  
...  
Keyword(s):  
Star Formation ◽  
Molecular Gas ◽  
Nearby Galaxies

scholarly journals The ALMaQUEST Survey – II. What drives central starbursts at z ∼ 0?

2020 ◽  
Vol 492 (4) ◽  
pp. 6027-6041 ◽  
Author(s):  
Sara L Ellison ◽  
Mallory D Thorp ◽  
Hsi-An Pan ◽  
Lihwai Lin ◽  
Jillian M Scudder ◽  
...  
Keyword(s):  
Star Formation ◽  
Surface Density ◽  
Stellar Mass ◽  
Starburst Galaxies ◽  
Molecular Gas ◽  
Central Regions ◽  
Primary Driver ◽  
Nearby Galaxies ◽  
Field Unit ◽  
Formation Efficiency

ABSTRACT Starburst galaxies have elevated star formation rates (SFRs) for their stellar mass. In Ellison et al., we used integral field unit maps of SFR surface density (ΣSFR) and stellar mass surface density (Σ⋆) to show that starburst galaxies in the local universe are driven by SFRs that are preferentially boosted in their central regions. Here, we present molecular gas maps obtained with the Atacama Large Millimeter Array (ALMA) observatory for 12 central starburst galaxies at z ∼ 0 drawn from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey. The ALMA and MaNGA data are well matched in spatial resolution, such that the ALMA maps of molecular gas surface density ($\Sigma _{\rm H_2}$) can be directly compared with MaNGA maps at kpc-scale resolution. The combination of $\Sigma _{\rm H_2}$, Σ⋆ and ΣSFR at the same resolution allow us to investigate whether central starbursts are driven primarily by enhancements in star formation efficiency (SFE) or by increased gas fractions. By computing offsets from the resolved Kennicutt-Schmidt relation ($\Sigma _{\rm H_2}$ versus ΣSFR) and the molecular gas main sequence (Σ⋆ versus $\Sigma _{\rm H_2}$), we conclude that the primary driver of the central starburst is an elevated SFE. We also show that the enhancement in ΣSFR is accompanied by a dilution in O/H, consistent with a triggering that is induced by metal poor gas inflow. These observational signatures are found in both undisturbed (9/12 galaxies in our sample) and recently merged galaxies, indicating that both interactions and secular mechanisms contribute to central starbursts.

scholarly journals CARMA SURVEY TOWARD INFRARED-BRIGHT NEARBY GALAXIES (STING): MOLECULAR GAS STAR FORMATION LAW IN NGC 4254

2011 ◽  
Vol 730 (2) ◽  
pp. 72 ◽  
Author(s):  
Nurur Rahman ◽  
Alberto D. Bolatto ◽  
Tony Wong ◽  
Adam K. Leroy ◽  
Fabian Walter ◽  
...  
Keyword(s):  
Star Formation ◽  
Molecular Gas ◽  
Nearby Galaxies

scholarly journals Influence of velocity dispersions on star-formation activities in galaxies

2020 ◽  
Vol 641 ◽  
pp. A24
Author(s):  
Tsan-Ming Wang ◽  
Chorng-Yuan Hwang
Keyword(s):  
Star Formation ◽  
High Velocity ◽  
Surface Density ◽  
Molecular Clouds ◽  
Velocity Dispersion ◽  
Power Index ◽  
Molecular Gas ◽  
Additional Parameter ◽  
Star Formation Activity ◽  
Nearby Galaxies

We investigated the influence of the random velocity of molecular gas on star-formation activities of six nearby galaxies. The physical properties of a molecular cloud, such as temperature and density, influence star-formation activities in the cloud. Additionally, local and turbulent motions of molecules in a cloud may exert substantial pressure on gravitational collapse and thus prevent or reduce star formation in the cloud. However, the influence of gas motion on star-formation activities remains poorly understood. We used data from the Atacama Large Millimeter/submillimeter Array to obtain 12CO(J = 1 − 0) flux and velocity dispersion. We then combined these data with 3.6 and 8 micron midinfrared data from the Spitzer Space Telescope to evaluate the effects of gas motion on star-formation activities in several nearby galaxies. We discovered that relatively high velocity dispersion in molecular clouds corresponds with relatively low star-formation activity. Considering the velocity dispersion as an additional parameter, we derived a modified Kennicutt-Schmidt law with a gas surface density power index of 0.84 and velocity dispersion power index of −0.61.

scholarly journals The effect of diffuse background on the spatially-resolved Schmidt relation in nearby spiral galaxies

2020 ◽  
Vol 634 ◽  
pp. A24 ◽  
Author(s):  
Nimisha Kumari ◽  
Mike J. Irwin ◽  
Bethan L. James
Keyword(s):  
Star Formation ◽  
Galaxy Formation ◽  
Spiral Galaxies ◽  
Formation Rate ◽  
Molecular Gas ◽  
Nearby Galaxy ◽  
Spatially Resolved ◽  
Diffuse Background ◽  
Nearby Galaxies ◽  
Atomic Gas

Context. The global Schmidt law of star formation provides a power-law relation between the surface densities of star-formation rate (SFR) and gas, and successfully explains plausible scenarios of galaxy formation and evolution. However, star formation being a multi-scale process, requires spatially-resolved analysis for a better understanding of the physics of star formation. Aims. It has been shown that the removal of a diffuse background from SFR tracers, such as Hα, far-ultraviolet (FUV), infrared, leads to an increase in the slope of the sub-galactic Schmidt relation. We reinvestigate the local Schmidt relations in nine nearby spiral galaxies taking into account the effect of inclusion and removal of diffuse background in SFR tracers as well as in the atomic gas. Methods. We used multiwavelength data obtained as part of the Spitzer Infrared Nearby Galaxies Survey, Key Insights on Nearby Galaxies: a Far-Infrared Survey with Herschel, The H I Nearby Galaxy Survey, and HERA CO-Line Extragalactic Survey. Making use of a novel split of the overall light distribution as a function of spatial scale, we subtracted the diffuse background in the SFR tracers as well as the atomic gas. Using aperture photometry, we study the Schmidt relations on background subtracted and unsubtracted data at physical scales varying between 0.5–2 kpc. Results. The fraction of diffuse background varies from galaxy to galaxy and accounts to ∼34% in Hα, ∼43% in FUV, ∼37% in 24 μm, and ∼75% in H I on average. We find that the inclusion of diffuse background in SFR tracers leads to a linear molecular gas Schmidt relation and a bimodal total gas Schmidt relation. However, the removal of diffuse background in SFR tracers leads to a super-linear molecular gas Schmidt relation. A further removal of the diffuse background from atomic gas results in a slope ∼1.4 ± 0.1, which agrees with dynamical models of star formation accounting for flaring effects in the outer regions of galaxies.

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