38 research outputs found
Interstellar H2 toward HD 37903
We present an analysis of interstellar H2 toward HD 37903, which is a hot, B
1.5 V star located in the NGC 2023 reflection nebula. Meyer et al. (2001) have
used a rich spectrum of vibrationally excited H2 observed by the HST to
calculate a model of the interstellar cloud toward HD 37903. We extend Mayer's
analysis by including the v"=0 vibrational level observed by the FUSE
satellite.
The T01 temperature should not be interpreted as a rotational temperature,
but rather as a temperature of thermal equilibrium between the ortho and para
H2. The ortho to para H2 ratio is lower for collisionally populated levels than
for the levels populated by fluorescence.
The PDR model of the cloud located in front of HD 37903 points to a gas
temperature Tkin=110-377 K, hydrogen density nH=1874-544 cm^-3 and the
star-cloud distance of 0.45 pc
Shocked Molecular Hydrogen in the 3C 326 Radio Galaxy System
The Spitzer spectrum of the giant FR II radio galaxy 3C 326 is dominated by
very strong molecular hydrogen emission lines on a faint IR continuum. The H2
emission originates in the northern component of a double-galaxy system
associated with 3C 326. The integrated luminosity in H2 pure-rotational lines
is 8.0E41 erg/s, which corresponds to 17% of the 8-70 micron luminosity of the
galaxy. A wide range of temperatures (125-1000 K) is measured from the H2 0-0
S(0)-S(7) transitions, leading to a warm H2 mass of 1.1E9 Msun. Low-excitation
ionic forbidden emission lines are consistent with an optical LINER
classification for the active nucleus, which is not luminous enough to power
the observed H2 emission. The H2 could be shock-heated by the radio jets, but
there is no direct indication of this. More likely, the H2 is shock-heated in a
tidal accretion flow induced by interaction with the southern companion galaxy.
The latter scenario is supported by an irregular morphology, tidal bridge, and
possible tidal tail imaged with IRAC at 3-9 micron. Unlike ULIRGs, which in
some cases exhibit H2 line luminosities of comparable strength, 3C 326 shows
little star-formation activity (~0.1 Msun/yr). This may represent an important
stage in galaxy evolution. Starburst activity and efficient accretion onto the
central supermassive black hole may be delayed until the shock-heated H2 can
kinematically settle and coolComment: 27 pages, 7 figures, accepted for publication in the Astrophysical
Journa
Mapping warm molecular hydrogen with Spitzer's Infrared Array Camera (IRAC)
Photometric maps, obtained with Spitzer's Infrared Array Camera (IRAC), can
provide a valuable probe of warm molecular hydrogen within the interstellar
medium. IRAC maps of the supernova remnant IC443, extracted from the Spitzer
archive, are strikingly similar to spectral line maps of the H2 pure rotational
transitions that we obtained with the Infrared Spectrograph (IRS) instrument on
Spitzer. IRS spectroscopy indicates that IRAC Bands 3 and 4 are indeed
dominated by the H2 v=0-0 S(5) and S(7) transitions, respectively. Modeling of
the H2 excitation suggests that Bands 1 and 2 are dominated by H2 v=1-0 O(5)
and v=0-0 S(9). Large maps of the H2 emission in IC433, obtained with IRAC,
show band ratios that are inconsistent with the presence of gas at a single
temperature. The relative strengths of IRAC Bands 2, 3, and 4 are consistent
with pure H2 emission from shocked material with a power-law distribution of
gas temperatures. CO vibrational emissions do not contribute significantly to
the observed Band 2 intensity. Assuming that the column density of H2 at
temperatures T to T+dT is proportional to T raised to the power -b for
temperatures up to 4000 K, we obtained a typical estimate of 4.5 for b. The
power-law index, b, shows variations over the range 3 to 6 within the set of
different sight-lines probed by the maps, with the majority of sight-lines
showing b in the range 4 to 5. The observed power-law index is consistent with
the predictions of simple models for paraboloidal bow shocks.Comment: 27 pages, including 11 figures. Accepted for publication in Ap
Interstellar H2 toward HD 147888
The ultraviolet and far--ultraviolet spectra of HD 147888 allows to access
the v=0 as well as higher vibrational levels of the ground H2 electronic level.
We have determined column densities of the H2 molecule on vibrational levels
v=0-5 and rotational levels J=0-6.
The ortho to para H2 ratio for the excited vibrational states equals to 1.2.
For the lowest vibrational state v=0 and rotational level J=1 the ortho to para
H2 ratio is only 0.16. The temperature of ortho-para thermodynamical
equilibrium is T_OP=43+-3 K.
The large number of H2 absorption lines in the HST spectra allows to
determine column densities even from a noisy spectra.
The measurements of H2 column densities on excited vibrational levels (from
the HST spectra) leads to constrains of radiation field in photon-dominated
regions (PDR) models of interstellar cloud towards HD 147888
Detection of Powerful Mid-IR H_2 Emission in the Bridge between the Taffy Galaxies
We report the detection of strong, resolved emission from warm H_2 in the Taffy galaxies and bridge. Relative to the continuum and faint polyclic aromatic hydrocarbon (PAH) emission, the H_2 emission is the strongest in the connecting bridge, approaching L(H_2)/L(PAH 8 μm) = 0.1 between the two galaxies, where the purely rotational lines of H_2 dominate the mid-infrared spectrum in a way very reminiscent of the group-wide shock in the interacting group Stephan's Quintet (SQ). The surface brightness in the 0-0 S(0) and S(1) H_2 lines in the bridge is more than twice that observed at the center of the SQ shock. We observe a warm H2 mass of 4.2 × 10^8 M_☉ in the bridge, but taking into account the unobserved bridge area, the total warm mass is likely to be twice this value. We use excitation diagrams to characterize the warm molecular gas, finding an average surface mass of ~5 × 10^6 M_☉ kpc^(–2) and typical excitation temperatures of 150-175 K. H_2 emission is also seen in the galaxy disks, although there the emission is more consistent with normal star-forming galaxies. We investigate several possible heating mechanisms for the bridge gas but favor the conversion of kinetic energy from the head-on collision via turbulence and shocks as the main heating source. Since the cooling time for the warm H_2 is short (~5000 yr), shocks must be permeating the molecular gas in the bridge region in order to continue heating the H_2
Kinematics and H_2 morphology of the multipolar Post-AGB star IRAS 16594-4656
context: The spectrum of IRAS 16594-4656 shows shock excited H_2 emission and
collisionally excited emission lines such as[O I],[C I],and [Fe II]. aim: The
goal is to determine the location of the H_2 and [Fe II] shock emission, to
determine the shock velocities,and constrain the physical properties in the
shock. methods: High resolution spectra of the H_2 1-0 S(1),H_2 2-1 S(1), [Fe
II], and Pa emission lines were obtained with the near infrared
spectrograph Phoenix on Gemini South. results: The position-velocity diagrams
of H_2 1-0 S(1), H_2 2-1 S(1), and [Fe II] are presented. The H_2 and [Fe II]
emission is spatially extended. The collisionally excited [O I] and [C I]
optical emission lines have a similar double peaked profile compared to the
extracted H_2 profile and appear to be produced in the same shock. They all
indicate an expansion velocity of ~8 km/s and the presence of a neutral, very
high density region with about 3 x 10^6 to 5 x10^7 cm. The
[Fe II] emission however is single peaked. It has a gaussian FWHM of 30 km/s
and a total width of 62 km/s at 1% of the peak. The Pa profile is even
wider with a gaussian FWHM of 48 km/s and a total width of 75 km/s at 1% of the
peak. conclusions: The H emission is excited in a slow 5 to 20 km/s shock
into dense material at the edge of the lobes, caused by the interaction of the
AGB ejecta and the post-AGB wind. The 3D representation of the H_2 data shows a
hollow structure with less H_2 emission in the equatorial region. The [Fe II]
emission is not present in the lobes, but originates close to the central star
in fast shocks in the post-AGB wind or in a disk. The Pa emission also
appears to originate close to the star.Comment: 11 pages and 8 figures; A&A in press; the paper includig high
resolution figures can be downloaded from
http://homepage.oma.be/gsteene/publications.htm
Molecular Hydrogen Excitation in Ultraluminous Infrared Galaxies
We report medium resolution VLT ISAAC K-band spectroscopy of the nuclei of
seven ultraluminous infrared galaxies. After accounting for stellar absorption
features, we have detected several molecular hydrogen (H_2) v=1-0, 2-1, and 3-2
vibrational emission lines, as well as the HI Br\gamma and HeI 2^1P-2^1S
recombination lines. The relative H_2 line intensities show little variation
between the objects, suggesting that the H_2 excitation mechanisms in the
nuclei are similar in all the objects. The 1-0 emissions appear thermalised at
temperatures T\sim1000K. However, the 2-1 and 3-2 emissions show evidence of
being radiatively excited by far-ultraviolet (FUV) photons, suggesting that the
H_2 excitation in the ULIRGs may arise in dense photon dominated regions
(PDRs). We show that the line ratios in the nuclei are consistent with PDRs
with cloud densities between 10^4 to 10^5cm^{-3}, exposed to far ultraviolet
(FUV) radiation fields at least 10^3 times more intense than the ambient FUV
intensity in the local interstellar medium. We have constructed starburst
models for the ULIRGs based on their H_2 properties, as well as on the
intensities of the recombination lines. Our models provide a consistent picture
of young 1-5Myr star clusters surrounded by relatively dense PDRs which are
irradiated by intense FUV fluxes. Comparison to the inner few hundred parsecs
of the Milky Way indicates that the star formation efficiency in ULIRGs is
10--100 times higher than in the Galactic Center.Comment: accepted by ApJ (32 pages including figures
Warm molecular hydrogen in the Spitzer SINGS galaxy sample
(simplified) Results on the properties of warm H2 in 57 normal galaxies are
derived from H2 rotational transitions, obtained as part of SINGS. This study
extends previous extragalactic surveys of H2, the most abundant constituent of
the molecular ISM, to more common systems (L_FIR = e7 to 6e10 L_sun) of all
morphological and nuclear types. The S(1) transition is securely detected in
the nuclear regions of 86% of SINGS galaxies with stellar masses above 10^9.5
M_sun. The derived column densities of warm H2 (T > ~100 K), even though
averaged over kiloparsec-scale areas, are commensurate with those of resolved
PDRs; the median of the sample is 3e20 cm-2. They amount to between 1% and >30%
of the total H2. The power emitted in the sum of the S(0) to S(2) transitions
is on average 30% of the [SiII] line power, and ~4e-4 of the total infrared
power (TIR) within the same area for star-forming galaxies, which is consistent
with excitation in PDRs. The fact that H2 emission scales tightly with PAH
emission, even though the average radiation field intensity varies by a factor
ten, can also be understood if both tracers originate predominantly in PDRs,
either dense or diffuse. A large fraction of the 25 LINER/Sy targets, however,
strongly depart from the rest of the sample, in having warmer H2 in the excited
states, and an excess of H2 emission with respect to PAHs, TIR and [SiII]. We
propose a threshold in H2 to PAH power ratios, allowing the identification of
low-luminosity AGNs by an excess H2 excitation. A dominant contribution from
shock heating is favored in these objects. Finally, we detect, in nearly half
the star-forming targets, non-equilibrium ortho to para ratios, consistent with
FUV pumping combined with incomplete ortho-para thermalization by collisions,
or possibly non-equilibrium PDR fronts advancing into cold gas.Comment: ApJS, in pres
Jet-Powered Molecular Hydrogen Emission from Radio Galaxies
H2 pure-rotational emission lines are detected from warm (100-1500 K)
molecular gas in 17/55 (31% of) radio galaxies at redshift z<0.22 observed with
the Spitzer IR Spectrograph. The summed H2 0-0 S(0)-S(3) line luminosities are
L(H2)=7E38-2E42 erg/s, yielding warm H2 masses up to 2E10 Msun. These radio
galaxies, of both FR radio morphological types, help to firmly establish the
new class of radio-selected molecular hydrogen emission galaxies (radio
MOHEGs). MOHEGs have extremely large H2 to 7.7 micron PAH emission ratios:
L(H2)/L(PAH7.7) = 0.04-4, up to a factor 300 greater than the median value for
normal star-forming galaxies. In spite of large H2 masses, MOHEGs appear to be
inefficient at forming stars, perhaps because the molecular gas is
kinematically unsettled and turbulent. Low-luminosity mid-IR continuum emission
together with low-ionization emission line spectra indicate low-luminosity AGNs
in all but 3 radio MOHEGs. The AGN X-ray emission measured with Chandra is not
luminous enough to power the H2 emission from MOHEGs. Nearly all radio MOHEGs
belong to clusters or close pairs, including 4 cool core clusters (Perseus,
Hydra, A 2052, and A 2199). We suggest that the H2 in radio MOHEGs is delivered
in galaxy collisions or cooling flows, then heated by radio jet feedback in the
form of kinetic energy dissipation by shocks or cosmic rays.Comment: ApJ in press, 40 pages, 18 figures, 14 table
Immunohistochemical staining of radixin and moesin in prostatic adenocarcinoma
<p>Abstract</p> <p>Background</p> <p>Some members of the Protein 4.1 superfamily are believed to be involved in cell proliferation and growth, or in the regulation of these processes. While the expression levels of two members of this family, radixin and moesin, have been studied in many tumor types, to our knowledge they have not been investigated in prostate cancer.</p> <p>Methods</p> <p>Tissue microarrays were immunohistochemically stained for either radixin or moesin, with the staining intensities subsequently quantified and statistically analyzed using One-Way ANOVA or nonparametric equivalent with subsequent Student-Newman-Keuls tests for multiple comparisons. There were 11 cases of normal donor prostates (NDP), 14 cases of benign prostatic hyperplasia (BPH), 23 cases of high-grade prostatic intraepithelial neoplasia (HGPIN), 88 cases of prostatic adenocarcinoma (PCa), and 25 cases of normal tissue adjacent to adenocarcinoma (NAC) analyzed in the microarrays.</p> <p>Results</p> <p>NDP, BPH, and HGPIN had higher absolute staining scores for radixin than PCa and NAC, but with a significant difference observed between only HGPIN and PCa (p = < 0.001) and HGPIN and NAC (p = 0.001). In the moesin-stained specimens, PCa, NAC, HGPIN, and BPH all received absolute higher staining scores than NDP, but the differences were not significant. Stage 4 moesin-stained PCa had a significantly reduced staining intensity compared to Stage 2 (p = 0.003).</p> <p>Conclusions</p> <p>To our knowledge, these studies represent the first reports on the expression profiles of radixin and moesin in prostatic adenocarcinoma. The current study has shown that there were statistically significant differences observed between HGPIN and PCa and HGPIN and NAC in terms of radixin expression. The differences in the moesin profiles by tissue type were not statistically significant. Additional larger studies with these markers may further elucidate their potential roles in prostatic neoplasia progression.</p