scholarly journals Molecular Gas Rich Galaxy Pair Unveiled in the Lensed Quasar 0957+561

2001 ◽  
Vol 205 ◽  
pp. 346-347
Author(s):  
P. Planesas ◽  
J. Martin-Pintado ◽  
R. Neri ◽  
L. Colina
Keyword(s):  
Host Galaxy ◽  
Molecular Gas ◽  
Gas Distribution ◽  
Companion Galaxy

Molecular gas in the host galaxy of the lensed quasar QSO 0957+561 has been detected at the redshift of 1.414 using the IRAM Plateau de Bure interferometer. This detection shows the extended nature of the molecular gas distribution. The molecular gas mass is 2-4 109 M⊙ and it is distributed in a disk that is several kiloparsecs in diameter. A second, weaker component of CO is interpreted as arising from a close companion galaxy moving at a velocity 440 km s−1 higher than the host galaxy.

scholarly journals BIMA Sub-arcsecond Carbon Monoxide Observations: Resolving the Inner kpc Region of the QSO I Zw 1

2001 ◽  
Vol 205 ◽  
pp. 340-343 ◽  
Author(s):  
Johannes Staguhn ◽  
Eva Schinnerer ◽  
Andreas Eckart
Keyword(s):  
Galaxy Formation ◽  
Angular Resolution ◽  
Line Emission ◽  
Host Galaxy ◽  
Molecular Gas ◽  
Nuclear Region ◽  
Gas Distribution ◽  
Multi Wavelength ◽  
Nearby Galaxies ◽  
Excitation Conditions

We present the first sub-kpc (∼ 0.7 ≈ 0.8 kpc) resolution 12CO(1–0) observations of the ISM in the host galaxy of the QSO I Zw 1 which were obtained with the BIMA mm-interferometer in its A configuration. The measurements, which are part of a multi-wavelength study of I Zw 1, will allow comparison of the ISM properties of a QSO host with those of nearby galaxies and place constraints on galaxy formation/evolution models. Our maps of the 12CO(1–0) line emission from the host galaxy of a QSO show a ring-like structure in the circumnuclear molecular gas distribution with a radius of about 900 pc. The presence of such a molecular gas ring was already predicted from earlier lower angular resolution PdBI observations (Schinnerer, Eckart, & Tacconi 1998). A first comparison of the BIMA data with new PdBI 12CO(2–1) observations with 0.9 angular resolution shows variations in the excitation conditions of the molecular gas in the innermost 3 comprising the nuclear region of I Zw 1.

scholarly journals Relativistic supernova 2009bb exploded close to an atomic gas cloud

2018 ◽  
Vol 618 ◽  
pp. A104 ◽  
Author(s):  
M. J. Michałowski ◽  
G. Gentile ◽  
T. Krühler ◽  
H. Kuncarayakti ◽  
P. Kamphuis ◽  
...  
Keyword(s):  
Star Formation ◽  
Main Sequence ◽  
Intergalactic Medium ◽  
Host Galaxy ◽  
Molecular Gas ◽  
Host Galaxies ◽  
Gas Distribution ◽  
Atomic Gas ◽  
First Time ◽  
Gas Properties

Context. The host galaxies of gamma-ray bursts (GRBs) have been claimed to have experienced a recent inflow of gas from the intergalactic medium. This is because their atomic gas distribution is not centred on their optical emission and because they are deficient in molecular gas given their high star formation rates (SFRs). Similar studies have not been conducted for host galaxies of relativistic supernovae (SNe), which may have similar progenitors. Aims. The potential similarity of the powering mechanisms of relativistic SNe and GRBs allowed us to make a prediction that relativistic SNe are born in environments similar to those of GRBs, that is, ones which are rich in atomic gas. Here we embark on testing this hypothesis by analysing the properties of the host galaxy NGC 3278 of the relativistic SN 2009bb. This is the first time the atomic gas properties of a relativistic SN host are provided and the first time resolved 21 cm-hydrogen-line (H I) information is provided for a host of an SN of any type in the context of the SN position. Methods. We obtained radio observations with the Australia Telescope Compact Array (ATCA) covering the H I line, and optical integral field unit spectroscopy observations with the Multi Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope (VLT). Moreover, we analysed archival carbon monoxide (CO) and multi-wavelength data for this galaxy. Results. The atomic gas distribution of NGC 3278 is not centred on the optical galaxy centre, but instead around a third of atomic gas resides in the region close to the SN position. This galaxy has a few times lower atomic and molecular gas masses than predicted from its SFR. Its specific SFR (sSFR ≡ SFR/M*) is approximately two to three times higher than the main-sequence value, placing it at the higher end of the main sequence, towards starburst galaxies. SN 2009bb exploded close to the region with the highest SFR density and the lowest age, as evident from high Hα EW, corresponding to the age of the stellar population of ~5.5 Myr. Assuming this timescale was the lifetime of the progenitor star, its initial mass would have been close to ~36 M⊙. Conclusions. As for GRB hosts, the gas properties of NGC 3278 are consistent with a recent inflow of gas from the intergalactic medium, which explains the concentration of atomic gas close to the SN position and the enhanced SFR. Super-solar metallicity at the position of the SN (unlike for most GRBs) may mean that relativistic explosions signal a recent inflow of gas (and subsequent star formation), and their type (GRBs or SNe) is determined either (i) by the metallicity of the inflowing gas, so that metal-poor gas results in a GRB explosion and metal-rich gas (for example a minor merger with an evolved galaxy or re-accretion of expelled gas) results in a relativistic SN explosion without an accompanying GRB, or (ii) by the efficiency of gas mixing (efficient mixing for SN hosts leading to a quick disappearance of metal-poor regions), or (iii) by the type of the galaxy (more metal-rich galaxies would result in only a small fraction of star formation being fuelled by metal-poor gas).

scholarly journals SMM J04135+10277: a distant QSO–starburst system caught by ALMA

2020 ◽  
Vol 493 (3) ◽  
pp. 3744-3756 ◽  
Author(s):  
Judit Fogasy ◽  
K K Knudsen ◽  
G Drouart ◽  
C D P Lagos ◽  
L Fan
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Spectral Energy Distribution ◽  
Line Emission ◽  
Continuum Emission ◽  
Host Galaxy ◽  
Spectral Energy ◽  
Molecular Gas ◽  
Gas Reservoir ◽  
Companion Galaxy

ABSTRACT The gas content of galaxies is a key factor for their growth, starting from star formation and black hole accretion to galaxy mergers. Thus, characterizing its properties through observations of tracers like the CO emission line is of big importance in order to understand the bigger picture of galaxy evolution. We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of dust continuum, CO(5–4) and CO(8–7) line emission in the quasar–star-forming companion system SMM J04135+10277 (z = 2.84). Earlier low-J CO studies of this system found a huge molecular gas reservoir associated with the companion galaxy, while the quasar appeared gas-poor. Our CO observations revealed that the host galaxy of the quasar is also gas-rich, with an estimated molecular gas mass of $\sim (0.7{\!-\!}2.3)\times 10^{10}\, \rm M_{\odot}$. The CO line profiles of the companion galaxy are very broad ($\sim 1000\, \rm km\, s^{-1}$), and show signs of rotation of a compact, massive system. In contrast to previous far-infrared observations, we resolve the continuum emission and detect both sources, with the companion galaxy dominating the dust continuum and the quasar having a $\sim 25{{\ \rm per\ cent}}$ contribution to the total dust emission. By fitting the infrared spectral energy distribution of the sources with mr-moose and empirical templates, the infrared luminosities of the quasar and the companion are in the range of $L_{\rm IR, QSO}\sim (2.1{\!-\!}9.6)\times 10^{12}\, \rm L_{\odot}$ and $L_{\rm IR, Comp.}\sim (2.4{\!-\!}24)\times 10^{12}\, \rm L_{\odot}$, while the estimated star formation rates are $\sim 210{\!-\!}960$ and $\sim 240{\!-\!}2400\, \rm M_{\odot }\, yr^{-1}$, respectively. Our results demonstrate that non-detection of low-J CO transition lines in similar sources does not necessarily imply the absence of massive molecular gas reservoir but that the excitation conditions favour the excitation of high-J transitions.

scholarly journals Molecular Gas Distribution in Barred and Nonbarred Galaxies along the Hubble Sequence

2008 ◽  
Vol 178 (2) ◽  
pp. 225-246 ◽  
Author(s):  
S. Komugi ◽  
Y. Sofue ◽  
K. Kohno ◽  
H. Nakanishi ◽  
S. Onodera ◽  
...  
Keyword(s):  
Molecular Gas ◽  
Gas Distribution ◽  
Hubble Sequence

scholarly journals Molecular gas in the host galaxy of a quasar at redshift z = 6.42

Nature ◽  
2003 ◽  
Vol 424 (6947) ◽  
pp. 406-408 ◽  
Author(s):  
Fabian Walter ◽  
Frank Bertoldi ◽  
Chris Carilli ◽  
Pierre Cox ◽  
K. Y. Lo ◽  
...  
Keyword(s):  
Host Galaxy ◽  
Molecular Gas

Dust-reddened Quasars

1996 ◽  
Vol 13 (2) ◽  
pp. 183-184 ◽  
Author(s):  
M. J. Drinkwater ◽  
R. L. Webster ◽  
P. J. Francis ◽  
T. Wiklind ◽  
F. Combes
Keyword(s):  
Molecular Clouds ◽  
Physical State ◽  
Absorption Lines ◽  
Line Of Sight ◽  
Host Galaxy ◽  
Molecular Gas ◽  
Molecular Absorption

We have recently discovered evidence for a population of radio-loud quasars that is reddened by dust. The dust is either along the line of sight to the quasars or is associated with the quasars. In the latter case the dust may be in molecular clouds in the quasar’s host galaxy, or in a molecular torus around the nucleus. We are planning to use 3 mm observations to search for molecular absorption lines (CO and HCO+) associated with dust at the redshift of these quasars. If any absorption systems are detected we will be able to deduce detailed information about the physical state of the molecular gas, hopefully showing which of the proposed locations of the dust is most likely.

scholarly journals Detection of 1.6 × 10 10 M ⊙ of Molecular Gas in the Host Galaxy of the z = 5.77 SDSS Quasar J0927+2001

2007 ◽  
Vol 666 (1) ◽  
pp. L9-L12 ◽  
Author(s):  
C. L. Carilli ◽  
R. Neri ◽  
R. Wang ◽  
P. Cox ◽  
F. Bertoldi ◽  
...  
Keyword(s):  
Host Galaxy ◽  
Molecular Gas

scholarly journals A DETECTION OF MOLECULAR GAS EMISSION IN THE HOST GALAXY OF GRB 080517

2014 ◽  
Vol 798 (1) ◽  
pp. L7 ◽  
Author(s):  
E. R. Stanway ◽  
A. J. Levan ◽  
N. R. Tanvir ◽  
K. Wiersema ◽  
T. P. R. van der Laan
Keyword(s):  
Host Galaxy ◽  
Molecular Gas ◽  
Gas Emission

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.

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