406 research outputs found
Arp 302: Non-starburst Luminous Infrared Galaxies
Arp 302, a luminous infrared source (L_{IR} = 4.2x10^{11} Lsun), consisting
of two spiral galaxies (VV340A and VV340B) with nuclear separation of 40'', has
the highest CO luminosity known. Observations with the BIMA array at 5'' X 7''
resolution reveal that the CO emission is extended over 23.0 kpc in the edge-on
spiral galaxy, VV340A, corresponding to 6.7x10^{10} Msun of H_2. In the
companion face-on galaxy, VV340B, the CO emission is extended over ~10.0 kpc,
with 1.1x10^{10} Msun of H_2. The large CO extent is in strong contrast to
starburst systems, such as Arp 220, in which the CO extent is typically 1
kpc. Furthermore, (H_2) is found to be 6.0 Lsun/Msun throughout
both galaxies. Thus the high IR luminosity of Arp 302 is apparently not due to
starbursts in the nuclear regions, but is due to its unusually large amount of
molecular gas forming stars at a rate similar to giant molecular clouds in the
Milky Way disk. Arp 302 consists of a pair of very gas-rich spiral galaxies
that may be interacting and in a phase before a likely onset of starbursts.Comment: AAS Latex plus two postscript figures. ApJ Letters (accepted
Single spin asymmetry measurements for inclusive productions in and \pi^-+\p_{\uparrow}\to \pi^0+X reactions at 70 and 40 GeV respectively
The inclusive asymmetries were measured in reactions and at 70 and 40 GeV/c respectively. The
measurements were made at the central region (for the first reaction) and
asymmetry is compatible with zero in the entire measured region. For the
second reaction the asymmetry is zero for small region () and increases with growth of . Averaged
over the interval the asymmetry was .Comment: 4 pages, 2 figures; Presented at SPIN-2004 at Trieste, October
10-16,200
Mapping IR Enhancements in Closely Interacting Spiral-Spiral Pairs. I. ISO~CAM and ISO~SWS Observations
Mid-infrared (MIR) imaging and spectroscopic observations are presented for a
well defined sample of eight closely interacting (CLO) pairs of spiral galaxies
that have overlapping disks and show enhanced far-infrared (FIR) emission. The
goal is to study the star formation distribution in CLO pairs, with special
emphasis on the role of 'overlap starbursts'. Observations were made with the
Infrared Space Observatory (ISO) using the CAM and SWS instruments. The ISO~CAM
maps, tracing the MIR emission of warm dust heated by young massive stars, are
compared to new ground based H and R-band images. We identify three
possible subgroups in the sample, classified according to the star formation
morphology: (1) advanced mergers (Arp~157, Arp~244 and Arp~299), (2) severely
disturbed systems (Arp~81 and Arp~278), and (3) less disturbed systems
(Arp~276, KPG 347 and KPG 426). Localized starbursts are detected in the
overlap regions in all five pairs of subgroups (1) and (2), suggesting that
they are a common property in colliding systems. Except for Arp~244, the
'overlap starburst' is usually fainter than the major nuclear starburst in CLO
pairs. Star formation in 'less disturbed systems' is often distributed
throughout the disks of both galaxies with no 'overlap starburst' detected in
any of them. These systems also show less enhanced FIR emission, suggesting
that they are in an earlier interaction stage than pairs of the other two
subgroups where the direct disk collisions have probably not yet occurred.Comment: 27 pages text, 4 JPEG figures, 3 PS figures. To be accepted by ApJ.
High quality figures (included in a PS file of the paper) can be found in
http://spider.ipac.caltech.edu/staff/cxu/papers/ss_iso.ps.g
Tower 1978
1978 yearbook of Westbrook College in Portland, Maine.https://dune.une.edu/wchc_yearbooks/1007/thumbnail.jp
Reversal of infall in SgrB2(M) revealed by Herschel/HIFI observations of HCN lines at THz frequencies
To investigate the accretion and feedback processes in massive star
formation, we analyze the shapes of emission lines from hot molecular cores,
whose asymmetries trace infall and expansion motions. The high-mass star
forming region SgrB2(M) was observed with Herschel/HIFI (HEXOS key project) in
various lines of HCN and its isotopologues, complemented by APEX data. The
observations are compared to spherically symmetric, centrally heated models
with density power-law gradient and different velocity fields (infall or
infall+expansion), using the radiative transfer code RATRAN. The HCN line
profiles are asymmetric, with the emission peak shifting from blue to red with
increasing J and decreasing line opacity (HCN to HCN). This is most
evident in the HCN 12--11 line at 1062 GHz. These line shapes are reproduced by
a model whose velocity field changes from infall in the outer part to expansion
in the inner part. The qualitative reproduction of the HCN lines suggests that
infall dominates in the colder, outer regions, but expansion dominates in the
warmer, inner regions. We are thus witnessing the onset of feedback in massive
star formation, starting to reverse the infall and finally disrupting the whole
molecular cloud. To obtain our result, the THz lines uniquely covered by HIFI
were critically important.Comment: A&A, HIFI special issue, accepte
Herschel observations of deuterated water towards Sgr B2(M)
Observations of HDO are an important complement for studies of water, because
they give strong constraints on the formation processes -- grain surfaces
versus energetic process in the gas phase, e.g. in shocks. The HIFI
observations of multiple transitions of HDO in Sgr~B2(M) presented here allow
the determination of the HDO abundance throughout the envelope, which has not
been possible before with ground-based observations only. The abundance
structure has been modeled with the spherical Monte Carlo radiative transfer
code RATRAN, which also takes radiative pumping by continuum emission from dust
into account. The modeling reveals that the abundance of HDO rises steeply with
temperature from a low abundance () in the outer envelope
at temperatures below 100~K through a medium abundance () in
the inner envelope/outer core, at temperatures between 100 and 200~K, and
finally a high abundance () at temperatures above 200~K in
the hot core.Comment: A&A HIFI special issue, accepte
SBS 0335-052, a probable nearby young dwarf galaxy: evidence pro and con
The results of Multiple Mirror Telescope spectrophotometry of the extremely
low-metallicity blue compact galaxy (BCG) SBS 0335-052 are presented. The
oxygen abundance in central brightest part of the galaxy is found to be 12 +
log(O/H) = 7.33+-0.01. The N/O, Ne/O, S/O and Ar/O abundance ratios are close
to those derived in other BCGs, suggesting that heavy element enrichment in the
HII region is due to massive star evolution. We detect auroral [OIII] 4363
emission in the inner part of HII region with a diameter of 3.6 kpc and find
that the HII region inside this diameter is hot, T_e~20000K. The oxygen
abundance in this region is nearly constant (12 + log(O/H) = 7.1 - 7.3),
implying effective mixing of ionized gas on short time-scales. We also discuss
the origin of blue underlying extended low-intensity emission detected in SBS
0335-052. The (V-I) and (R-I) color distributions suggest that a significant
contribution to the extended envelope is due to ionized gas emission. However,
the observed equivalent width of Hbeta emission in the extended envelope is 2-3
times lower than the value expected in the case of pure gaseous emission. These
findings suggest that, along with the blue young (~10^7yr) stellar clusters, an
older stellar population with age ~10^8yr may be present in the extended
envelope of SBS 0335-052, having a total mass conclude that SBS 0335-052 is a
young nearby dwarf galaxy with age ~10^8 yr.Comment: 27 pages and 8 Postscript figures, uses aaspp4.sty. Submitted to
Astrophysical Journa
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