45 research outputs found
Threshold between Spontaneous and Cloud-Collisional Star Formation
Based on simple physical and geometric assumptions, we have calculated the
mean surface molecular density of spiral galaxies at the threshold between star
formation induced by cloud-cloud collision and spontaneous gravitational
collapse. The calculated threshold is approximately , where \Sigma \quad \mathrm{M_{\solar}}\cdot \mathrm{pc}^{-2} is
the observed surface mass density of an assumed flat gas disk. Above this
limit, the rate of molecular cloud collisions dominates over spontaneous
molecular cloud collapse. This model may explain the apparent discontinuity in
the Schmidt law found recently at .Comment: Accepted for publication in PAS
The Schmidt Law at High Molecular Densities
We have combined Halpha and recent high resolution CO(J=1-0) data to consider
the quantitative relation between gas mass and star formation rate, or the
so-called Schmidt law in nearby spiral galaxies at regions of high molecular
density. The relation between gas quantity and star formation rate has not been
previously studied for high density regions, but using high resolution CO data
obtained at the NMA(Nobeyama Millimeter Array), we have found that the
Schmidt law is valid at densities as high as for the sample spiral galaxies, which is an order of
magnitude denser than what has been known to be the maximum density at which
the empirical law holds for non-starburst galaxies. Furthermore, we obtain a
Schmidt law index of and roughly constant star formation
efficiency over the entire disk, even within the several hundred parsecs of the
nucleus. These results imply that the physics of star formation does not change
in the central regions of spiral galaxies. Comparisons with starburst galaxies
are also given. We find a possible discontinuity in the
Schmidt law between normal and starburst galaxies
12CO and 13CO observation of the low-metallicity dwarf galaxy DDO 154
The conversion factor from carbon monoxide (CO) intensity to molecular gas
mass is a source of large uncertainty in understanding gas and its relation to
star formation in galaxies. In particular, the conversion factor in low
metallicity environments have remained elusive, as currently only two galaxies
have been detected in any CO isotopes in environments with 12+log (O/H) < 8.0.
Here we report 12CO(J=1-0) and 13CO(J=1-0) observations towards a star forming
region in DDO 154, a low metallicity dwarf irregular galaxy at 12+log (O/H) =
7.67. This is a re-observation of a previous non-detection at higher angular
and velocity resolution. No significant emission was detected. By estimating
the molecular gas mass from associated star formation, we find that DDO 154 has
a conversion factor of more than 10^3 times the Milky Way. Alternatively, if we
estimate molecular mass using dust continuum emission, the conversion factor is
at least 2 orders of magnitude larger than the Milky Way. These estimates
signify a large amount of CO-dark molecular gas in this galaxy.Comment: 7 pages, 2 figures, published in Publications of the Astronomical
Society of Japan (PASJ
Deep CO Observations and the CO-to-H_2 Conversion Factor in DDO 154, a Low Metallicity Dwarf Irregular Galaxy
We present a deep spectroscopic search for CO emission in the dwarf irregular
galaxy DDO154, which has an Oxygen abundance of only 1/20 the solar value. The
observations were conducted in order to constrain the CO-to-
conversion factor at low metallicity. No CO was detected, however, despite
being one of the sensitive observations done towards galaxies of this type. We
succeed in putting a strong lower limit on the conversion factor, at least 10
times the Galactic value. Our result supports previous studies which argue for
a high conversion factor at low metallicity.Comment: 11 pages, 4 figures. Accepted for publication in PAS
ASTE observations of nearby galaxies: A tight correlation between CO(J=3-2) emission and Halpha
Star formation rates (SFRs) obtained via extinction corrected H alpha are
compared to dense gas as traced by CO(J=3-2) emission at the centers of nearby
galaxies, observed with the ASTE telescope. It is found that, although many of
the observed positions are dusty and therefore heavily absorbed at H alpha, the
SFR shows a striking correlation with dense gas in the form of the Schmidt law
with an index 1.0. The correlation is also compared between gas traced by
CO(J=1-0) and application of H alpha extinction correction. We find that dense
gas produces a far better correlation with SFR in view of surface density
values.Comment: 6 pages, PASJ accepte
Detection of extended millimeter emission in the host galaxy of 3C273 and its implications for QSO feedback via high dynamic range ALMA imaging
We estimate the amount of negative feedback energy injected into the ISM of
the host galaxy of 3C273, a prototypical radio loud quasar. We obtained 93, 233
and 343 GHz continuum images with the Atacama Large Millimeter/Sub-millimeter
Array (ALMA). After self calibration and point source subtraction, we reach an
image dynamic range of at 93\ GHz, at 233\ GHz and
at 343\ GHz. These are currently the highest image dynamic range
obtained using ALMA. We detect spatially extended millimeter emission
associated with the host galaxy, cospatial with the Extended Emission Line
Region (EELR) observed in the optical. The millimeter spectral energy
distribution and comparison with centimeter data show that the extended
emission cannot be explained by dust thermal emission, synchrotron or thermal
bremsstrahlung arising from massive star formation. We interpret the extended
millimeter emission as thermal bremsstrahlung from gas directly ionized by the
central source. The extended flux indicates that at least of the
bolometric flux of the nuclear source was used to ionize atomic hydrogen in the
host galaxy. The ionized gas is estimated to be as massive as to
, but the molecular gas fraction with respect to the
stellar mass is consistent with other ellipticals, suggesting that direct
ionization ISM by the QSO may not be sufficient to suppress star formation, or
we are witnessing a short timescale before negative feedback becomes
observable. The discovery of a radio counterpart to EELRs provides a new
pathway to studying the QSO-host ISM interaction
13CO(J=1-0) On-the-fly Mapping of the Giant HII Region NGC 604: Variation in Molecular Gas Density and Temperature due to Sequential Star Formation
We present 13CO(J=1-0) line emission observations with the Nobeyama 45-m
telescope toward the giant HII region NGC 604 in the spiral galaxy M 33. We
detected 13CO(J=1-0) line emission in 3 major giant molecular clouds (GMCs)
labeled as GMC-A, B, and C beginning at the north. We derived two line
intensity ratios, 13CO(J=1-0)/12CO(J =1-0), R13/12, and 12CO(J=3-2)/12CO(J
=1-0), R31, for each GMC at an angular resolution of 25" (100 pc). Averaged
values of R13/12 and R31 are 0.06 and 0.31 within the whole GMC-A, 0.11 and
0.67 within the whole GMC-B, and 0.05 and 0.36 within the whole GMC-C,
respectively. In addition, we obtained R13/12=0.09\pm0.02 and R31=0.76\pm0.06
at the 12CO(J=1-0) peak position of the GMC-B. Under the Large Velocity
Gradient approximation, we determined gas density of 2.8 \times10^3 cm^-3 and
kinetic temperature of 33+9-5 K at the 12CO(J=1-0) peak position of the GMC-B.
Moreover, we determined 2.5 \times10^3 cm^-3 and 25\pm2 K as averaged values
within the whole GMC-B. We concluded that dense molecular gas is formed
everywhere in the GMC-B because derived gas density not only at the peak
position of the GMC but also averaged over the whole GMC exceeds 10^3 cm^-3. On
the other hand, kinetic temperature averaged over the whole GM-B, 25 K, is
significantly lower than that at the peak position, 33 K. This is because HII
regions are lopsided to the northern part of the GMC-B, thus OB stars can heat
only the northern part, including the 12CO(J=1-0) peak position, of this GMC.Comment: 16 pages, 7 figures, PASJ in pres