Vig S.,Indian Institute of Space Science and Technology |
Testi L.,National institute for astrophysics |
Testi L.,European Southern Observatory |
Walmsley C.M.,National institute for astrophysics |
And 3 more authors.
Astronomy and Astrophysics | Year: 2017
Context. Since massive and intermediate mass stars form in clusters, a comparative investigation of the environments of the young embedded cluster members can reveal significant information about the conditions under which stars form and evolve. Aims. IRAS 18511+0146 is a young embedded (proto)cluster located at 3.5 kpc surrounding what appears to be an intermediate mass protostar. Here, we investigate the nature of cluster members (two of which are believed to be the most massive and luminous) using imaging and spectroscopy in the near and mid-infrared. In particular, we examine the three brightest mid-infrared objects, two of which are believed to be the most massive ones driving the luminosity of this region. Methods. Near-infrared spectroscopy of nine objects (bright in K-bands) towards IRAS 18511+0146 has been carried out. Several cluster members have also been investigated in the mid-infrared using spectroscopic and imaging with VISIR on the VLT. Far-infrared images from the Herschel Hi-GAL survey have been used to construct the column density and temperature maps of the region. Results. The brightest point-like object associated with IRAS 18511+0146 is referred to as S7 in the present work (designated UGPS J185337.88+015030.5 in the UKIRT Galactic Plane survey). S7 is likely the most luminous object in the cluster as it is bright at all wavelengths ranging from the near-infrared to millimetre. Seven of the nine objects show rising spectral energy distributions in the near-infrared, with four objects showing Br-γ emission. Three members: S7, S10 (also UGPS J185338.37+015015.3) and S11 (also UGPS J185338.72+015013.5) are bright in mid-infrared with diffuse emission being detected in the vicinity of S11 in PAH bands. Silicate absorption is detected towards these three objects, with an absorption maximum between 9.6 and 9.7 μm, large optical depths (1.8-3.2), and profile widths of 1.6-2.1μm. The silicate profiles of S7 and S10 are similar, in contrast to S11 (which has the largest width and optical depth). The cold dust emission peaks at S7, with temperature at 26 K and column density N(H2) ∼ 7 × 1022 cm-2. The bolometric luminosity of IRAS 18511 region is L ∼ 1.8 × 104L⊙. S7 is the main contributor to the bolometric luminosity, with L (S7) ≳ 104L⊙. Conclusions. S7 is a high-mass protostellar object with ionised stellar winds, evident from the correlation between radio and bolometric luminosity, as well as the asymmetric Br-γ profile. The differences in silicate profiles of S7 and S11 could be due to different radiation environments as we believe the former to be more massive and in an earlier phase than the latter. © ESO, 2017.
Padovani M.,Institute Of Ciancies Of Lespai Csicieec |
Walmsley C.M.,INAFOsservatorio Astrofisico di Arcetri |
Walmsley C.M.,Dublin Institute of Advanced Studies |
Tafalla M.,Observatorio Astronmico Nacional IGN |
And 3 more authors.
Astronomy and Astrophysics | Year: 2011
Aims. We studied the abundance of HCN, H13CN, and HN 13C in a sample of prestellar cores, in order to search for species associated with high density gas. Methods. We used the IRAM 30 m radiotelescope to observe along the major and the minor axes of L1498, L1521E, and TMC 2, three cores chosen on the basis of their CO depletion properties. We mapped the J = 1 → 0 transition of HCN, H13CN, and HN13C towards the source sample plus the J = 1 → 0 transition of N2H+ and the J = 2 → 1 transition of C18O in TMC 2. We used two different radiative transfer codes, making use of recent collisional rate calculations, in order to determine more accurately the excitation temperature, leading to a more exact evaluation of the column densities and abundances. Results. We find that the optical depths of both H13CN(1-0) and HN13C(1-0) are non-negligible, allowing us to estimate excitation temperatures for these transitions in many positions in the three sources. The observed excitation temperatures are consistent with recent computations of the collisional rates for these species and they correlate with hydrogen column density inferred from dust emission. We conclude that HCN and HNC are relatively abundant in the high density zone, n(H2) ∼ 105 cm-3, where CO is depleted. The relative abundance [HNC]/[HCN] differs from unity by at most 30% consistent with chemical expectations. The three hyperfine satellites of HCN(1-0) are optically thick in the regions mapped, but the profiles become increasingly skewed to the blue (L1498 and TMC 2) or red (L1521E) with increasing optical depth suggesting absorption by foreground layers. © 2011 ESO.
Dolan B.P.,National University of Ireland, Maynooth |
Dolan B.P.,Dublin Institute of Advanced Studies |
Szabo R.J.,Heriot - Watt University |
Szabo R.J.,Maxwell Institute for Mathematical science
Physical Review D - Particles, Fields, Gravitation and Cosmology | Year: 2013
We study vacuum states and symmetric fermions in the equivariant dimensional reduction of the Yang-Mills-Dirac theory over the six-dimensional homogeneous space SU(3)/U(1)×U(1) endowed with a family of SU(3) structures including a nearly Kähler structure. We derive the fixed tree-level scalar potentials of the induced Yang-Mills-Higgs theory and compute the dynamically generated gauge and Higgs boson masses as functions of the metric moduli of the coset space. We find an integrable subsector of the Higgs field theory that is governed by a sine-Gordon-type model whose topological soliton solutions are determined nonperturbatively by the gauge coupling and that tunnel between families of infinitely degenerate vacua. The reduction of the Dirac action for symmetric fermions yields exactly massless chiral fermions containing subsectors that have fixed tree-level Yukawa interactions. We compute dynamical fermion mass matrices explicitly and compare them at different points of the moduli space, some of which support consistent heterotic flux vacua. © 2013 American Physical Society.
Wienen M.,Max Planck Institute for Radio Astronomy |
Wyrowski F.,Max Planck Institute for Radio Astronomy |
Schuller F.,Max Planck Institute for Radio Astronomy |
Menten K.M.,Max Planck Institute for Radio Astronomy |
And 4 more authors.
Astronomy and Astrophysics | Year: 2012
Context. The APEX Telescope Large Area Survey: the GALaxy (ATLASGAL) is an unbiased continuum survey of the inner Galactic disk at 870 μm. It covers ±60° in Galactic longitude and aims to find all massive clumps at various stages of high-mass star formation in the inner Galaxy, particularly the earliest evolutionary phases. Aims. We aim to determine properties such as the gas kinetic temperature and dynamics of new massive cold clumps found by ATLASGAL. Most importantly, we derived their kinematical distances from the measured line velocities. Methods. We observed the ammonia (J,K) = (1, 1) to (3, 3) inversion transitions toward 862 clumps of a flux-limited sample of submm clumps detected by ATLASGAL and extracted 13CO (1-0) spectra from the Galactic Ring Survey (GRS). We determined distances for a subsample located at the tangential points (71 sources) and for 277 clumps whose near/far distance ambiguity is resolved. Results. Most ATLASGAL clumps are cold with rotational temperatures from 10-30 K with a median of 17 K. They have a wide range of NH 3 linewidths (1-7 km s -1) with 1.9 km s -1 as median, which by far exceeds the thermal linewidth, as well as a broad distribution of high column densities from 10 14 to 10 16 cm -2 (median of 2 × 10 15 cm -2) with an NH 3 abundance in the range of 5 to 30 × 10 -8. ATLASGAL sources are massive, ≳ 100 M, and a fraction of clumps with a broad linewidth is in virial equilibrium. We found an enhancement of clumps at Galactocentric radii of 4.5 and 6 kpc. The comparison of the NH 3 lines as high-density probes with the GRS 13CO emission as low-density envelope tracer yields broader linewidths for 13CO than for NH 3. The small differences in derived clump velocities between NH 3 (representing dense core material) and 13CO (representing more diffuse molecular cloud gas) suggests that the cores are essentially at rest relative to the surrounding giant molecular cloud. Conclusions. The high detection rate (87%) confirms ammonia as an excellent probe of the molecular content of the massive, cold clumps revealed by ATLASGAL. A clear trend of increasing rotational temperatures and linewidths with evolutionary stage is seen for source samples ranging from 24 μm dark clumps to clumps with embedded HII regions. The survey provides the largest ammonia sample of high-mass star forming clumps and thus presents an important repository for the characterization of statistical properties of the clumps and the selection of subsamples for detailed, high-resolution follow-up studies. © 2012 ESO.
Merello M.,University of Chile |
Merello M.,University of Texas at Austin |
Bronfman L.,University of Chile |
Garay G.,University of Chile |
And 4 more authors.
Astrophysical Journal | Year: 2013
We report molecular line and dust continuum observations toward the high-mass star-forming region G331.5-0.1, one of the most luminous regions of massive star formation in the Milky Way, located at the tangent region of the Norma spiral arm, at a distance of 7.5 kpc. Molecular emission was mapped toward the G331.5-0.1 GMC in the CO(J = 1 → 0) and C18O(J = 1 → 0) lines with NANTEN, while its central region was mapped in CS(J = 2 → 1 and J = 5 → 4) with SEST, and in CS(J = 7 → 6) and 13CO(J = 3 → 2) with ASTE. Continuum emission mapped at 1.2 mm with SIMBA and at 0.87 mm with LABOCA reveal the presence of six compact and luminous dust clumps, making this source one of the most densely populated central regions of a GMC in the Galaxy. The dust clumps are associated with molecular gas and they have the following average properties: size of 1.6 pc, mass of 3.2 × 10 3 M ⊙, molecular hydrogen density of 3.7 × 104 cm-3, dust temperature of 32 K, and integrated luminosity of 5.7 × 105 L⊙, consistent with values found toward other massive star-forming dust clumps. The CS and 13CO spectra show the presence of two velocity components: a high-velocity component at -89 km s-1, seen toward four of the clumps, and a low-velocity component at -101 km s-1 seen toward the other two clumps. Radio continuum emission is present toward four of the molecular clumps, with spectral index estimated for two of them of 0.8 ± 0.2 and 1.2 ± 0.2. A high-velocity molecular outflow is found at the center of the brightest clump, with a line width of 26 km s-1 (FWHM) in CS(J = 7 → 6). Observations of SiO(J = 7 → 6 and J = 8 → 7), and SO(JK = 88 → 77 and JK = 87 → 76) lines provide estimates of the gas rotational temperature toward this outflow >120 K and >75 K, respectively. © 2013. The American Astronomical Society. All rights reserved.
Gallerani S.,National institute for astrophysics |
Gallerani S.,Institut Universitaire de France |
Neri R.,Institut Universitaire de France |
Maiolino R.,National institute for astrophysics |
And 12 more authors.
Astronomy and Astrophysics | Year: 2012
We present one of the first resolved maps of the [CII] 158 μm line, a powerful tracer of the star forming inter-stellar medium, at high redshift. We use the new IRAM PdBI receivers at 350 GHz to map this line in BRI 0952-0115, the host galaxy of a lensed quasar at z = 4.4 previously found to be very bright in [CII] emission. The [CII] emission is clearly resolved and our data allow us to resolve two [CII] lensed images associated with the optical quasar images. We find that the star formation, as traced by [CII], is distributed over a region of about 1 kpc in size near the quasar nucleus, and we infer a star formation surface density 150 M· yr-1 kpc -2, similar to that observed in local ULIRGs. We also reveal another [CII] component, extended over ~12 kpc, and located at about 10 kpc from the quasar. We suggest that this component is a companion disk galaxy, in the process of merging with the quasar host, whose rotation field is distorted by the interaction with the quasar host, and where star formation, although intense, is more diffuse. These observations suggest that galaxy merging at high-z can enhance star formation at the same time in the form of more compact regions, in the vicinity of the accreting black hole, and in more extended star forming galaxies. © 2012 ESO.
Becker T.W.,University of Southern California |
Schaeffer A.J.,Dublin Institute of Advanced Studies |
Lebedev S.,Dublin Institute of Advanced Studies |
Conrad C.P.,University of Hawaii at Manoa
Geophysical Research Letters | Year: 2015
An absolute plate motion (APM) model is required to address issues such as the thermochemical evolution of Earth's mantle. All APM models have to rely on indirect inferences, including those based on hot spots and seismic anisotropy, each with their own set of uncertainties. Here, we explore a seafloor spreading-aligned reference frame. We show that this reference frame fits azimuthal seismic anisotropy in the uppermost mantle very well. The corresponding Euler pole is close to those of hot spot reference frames, ridge motion minimizing models, and geodynamic estimates of net rotation and predicts clear trench motion patterns. We conclude that a net rotation pole guided by the spreading-aligned model (at 64°E, 61°S, with moderate rotation of ∼ 0.2 ... 0.3°/Myr) could indeed represent a standard, comprehensive reference frame for present-day plate motions with respect to the deep mantle. Key Points A spreading-aligned plate motion reference frame matches seismic anisotropy This defines a comprehensive reference frame matching hot spots Universal reference frame clarifies subduction zone trench migration ©2015. American Geophysical Union. All Rights Reserved.
Ambrogi L.,University of L'Aquila |
De Ona Wilhelmi E.,Institute for Space science CSIC IEEC |
Aharonian F.,University of L'Aquila |
Aharonian F.,Dublin Institute of Advanced Studies |
Aharonian F.,Max Planck Institute for Nuclear Physics
Astroparticle Physics | Year: 2016
The potential of an array of imaging atmospheric Cherenkov telescopes to detect gamma-ray sources in complex regions has been investigated. The basic characteristics of the gamma-ray instrument have been parameterized using simple analytic representations. In addition to the ideal (Gaussian form) point spread function (PSF), the impact of more realistic non-Gaussian PSFs with tails has been considered. Simulations of isolated point-like and extended sources have been used as a benchmark to test and understand the response of the instrument. The capability of the instrument to resolve multiple sources has been analyzed and the corresponding instrument sensitivities calculated. The results are of particular interest for weak gamma-ray emitters located in crowded regions of the Galactic plane, where the chance of clustering of two or more gamma-ray sources within 1 deg is high. © 2016 Elsevier B.V. All rights reserved.
Leurini S.,Max Planck Institute for Radio Astronomy |
Menten K.M.,Max Planck Institute for Radio Astronomy |
Walmsley C.M.,National institute for astrophysics |
Walmsley C.M.,Dublin Institute of Advanced Studies
Astronomy and Astrophysics | Year: 2016
Context. Class I methanol masers are thought to be tracers of interstellar shock waves. However, they have received relatively little attention mostly as a consequence of their low luminosities compared to other maser transitions. This situation has changed recently and Class I methanol masers are now routinely used as signposts of outflow activity especially in high extinction regions. The recent detection of polarisation in Class I lines now makes it possible to obtain direct observational information about magnetic fields in interstellar shocks. Aims. We make use of newly calculated collisional rate coefficients for methanol to investigate the excitation of Class I methanol masers and to reconcile the observed Class I methanol maser properties with model results. Methods.We performed large velocity gradient calculations with a plane-parallel slab geometry appropriate for shocks to compute the pump and loss rates which regulate the interactions of the different maser systems with the maser reservoir. We study the dependence of the pump rate coefficient, the maser loss rate, and the inversion efficiency of the pumping scheme of several Class I masers on the physics of the emitting gas. Results. We predict inversion in all transitions where maser emission is observed. Bright Class I methanol masers are mainly hightemperature (>100 K) high-density (n(H2) 107-108 cm-3) structures with methanol maser emission measures, corresponding to high methanol abundances close to the limits set by collisional quenching. Our model predictions reproduce reasonably well most of the observed properties of Class I methanol masers. Class I masers in the 25 GHz series are the most sensitive to the density of the medium and mase at higher densities than other lines. Moreover, even at high density and high methanol abundances, their luminosity is predicted to be lower than that of the 44 GHz and 36 GHz masers. Our model predictions also reflect the observational result that the 44 GHz line is almost always stronger than the 36 GHz maser. By comparison between observed isotropic photon luminosities and our model predictions, we infer maser beam solid angles of roughly 10-3 steradian. Conclusions. We find that the Class I masers can reasonably be separated into three families: the (J + 1)-1 - J0-E type series, the (J + 1)0 - J1-A type, and the J2 - J1-E lines at 25 GHz. The 25 GHz lines behave in a different fashion from the other masers as they are only inverted at high densities above 106 cm-3 in contrast to other Class I masers. Therefore, the detection of maser activity in all three families is a clear indication of high densities. © ESO 2016.
Crocker R.M.,Australian National University |
Bicknell G.V.,Australian National University |
Taylor A.M.,Dublin Institute of Advanced Studies |
Carretti E.,National institute for astrophysics |
Astrophysical Journal | Year: 2015
The Galactic center's giant outflows are manifest in three different, nonthermal phenomena: (1) the hard-spectrum, γ-ray "Fermi bubbles" emanating from the nucleus and extending to |b| ∼ 50°; (2) the hard-spectrum, total-intensity microwave (∼20-40 GHz) "haze" extending to |b| ∼ 35° in the lower reaches of the Fermi bubbles; and (3) the steep-spectrum, polarized, "S-PASS" radio (∼2-20 GHz) lobes that envelop the bubbles and extend to |b|∼ 60°. We find that the nuclear outflows inflate a genuine bubble in each Galactic hemisphere that has the classical structure, working outward, of reverse shock, contact discontinuity (CD), and forward shock. Expanding into the finite pressure of the halo and given appreciable cooling and gravitational losses, the CD of each bubble is now expanding only very slowly. We find observational signatures in both hemispheres of giant, reverse shocks at heights of ∼1 kpc above the nucleus; their presence ultimately explains all three of the nonthermal phenomena mentioned above. Synchrotron emission from shock-reaccelerated cosmic-ray electrons explains the spectrum, morphology, and vertical extent of the microwave haze and the polarized radio lobes. Collisions between shock-reaccelerated hadrons and denser gas in cooling condensations that form inside the CD account for most of the bubbles' γ-ray emissivity. Inverse Compton emission from primary electrons contributes at the 10%-30% level. Our model suggests that the bubbles are signatures of a comparatively weak but sustained nuclear outflow driven by Galactic center star formation over few × 108 yr. © 2015. The American Astronomical Society. All rights reserved.