A5049237428- Astrophysics and Star Formation Studies
- Stellar, planetary, and galactic studies
- Astro and Planetary Science
- Molecular Spectroscopy and Structure
- Astronomical Observations and Instrumentation
- Astronomy and Astrophysical Research
- Atmospheric Ozone and Climate
- Astrophysical Phenomena and Observations
- History and Developments in Astronomy
- Experimental and Theoretical Physics Studies
- Historical Astronomy and Related Studies
- Galaxies: Formation, Evolution, Phenomena
- Historical Geography and Cartography
- Calibration and Measurement Techniques
- Space Exploration and Technology
- Adaptive optics and wavefront sensing
- Spacecraft Design and Technology
- Gamma-ray bursts and supernovae
- Aerospace Engineering and Energy Systems
- Advanced Combustion Engine Technologies
- Spectroscopy and Laser Applications
- Phase Equilibria and Thermodynamics
- Spacecraft Dynamics and Control
- Particle Accelerators and Free-Electron Lasers
- Historical and Architectural Studies
Max Planck Institute for Astronomy
2007-2017
Heidelberg University
2017
Max Planck Society
2010-2015
PC Krause & Associates (United States)
2010
Private University College of Education of the Diocese of Linz
2010
Ruhr University Bochum
1997-2007
European Southern Observatory
2001-2003
The Photodetector Array Camera and Spectrometer (PACS) is one of the three science instruments on ESA's far infrared submillimetre observatory. It employs two Ge:Ga photoconductor arrays (stressed unstressed) with 16x25 pixels, each, filled silicon bolometer 16x32 32x64 respectively, to perform integral-field spectroscopy imaging photometry in 60-210μ m wavelength regime. In mode, it simultaneously images bands, 60-85μ or 85-125μ\m 125-210μ m, over a field view ~1.75'x3.5', close Nyquist...
Context. The temperature and density structure of molecular cloud cores are the most important physical quantities that determine course protostellar collapse properties stars they form. Nevertheless, profiles often rely either on simplifying assumption isothermality or observationally poorly constrained model profiles. instruments Herschel satellite provide us for first time with both spectral coverage spatial resolution is needed to directly measure dust nearby cores.
Context. Stars are born deeply embedded in molecular clouds. In the earliest phases, protostars emit bulk of their radiation far-infrared wavelength range, where Herschel is perfectly suited to probe at high angular resolution and dynamic range. high-mass regime, birthplaces thought be high-density structures known as infrared-dark clouds (IRDCs). While massive IRDCs believed have right conditions give rise stars clusters, evolutionary sequence this process not well-characterized.
<i>Context. <i/>Infrared-dark clouds (IRDCs) are the precursors to massive stars and stellar clusters. G011.11–0.12 is a well-studied filamentary IRDC, though, date, absence of far-infrared data with sufficient spatial resolution has limited understanding structure star-formation activity.<i>Aims. <i/>We use <i>Herschel<i/> study embedded population young pre- protostellar cores in this IRDC. <i>Methods. examine cloud structure, which appears absorption at short wavelength emission longer...
(Abriged) In the framework of Herschel GTKP "The earliest phases star formation", we have imaged B68 between 100 and 500 um. Ancillary (sub)mm data, spectral line maps 12/13CO(2-1) transitions as well a NIR extinction map were added to analysis. We employed ray-tracing algorithm derive 2D mid-plane dust temperature volume density distribution without suffering from LoS averaging effects simple SED fitting procedures. Additional 3D radiative transfer calculations investigate connection...
Aims: We study the fragmentation and dynamical properties of a massive starless gas clump at onset high-mass star formation. Methods: Based on Herschel continuum data we identify that remains far-infrared dark up to 100mum wavelengths. The are investigated by means Plateau de Bure Interferometer Nobeyama 45m single-dish spectral line observations. Results: reservoir fragments spatial scales ~18000AU in four cores. Comparing extent this region with intermediate- low-mass cores from...
We present <i>Herschel<i/> observations of the isolated, low-mass star-forming Bok globule CB244. It contains two cold sources, a Class 0 protostar and starless core, which is likely to be prestellar in nature, separated by 90 (~18 000 AU). The data sample peak <i>Planck<i/> spectrum for these are therefore ideal dust-temperature column density modeling. With near-IR extinction map, MIPS 70 <i>μ<i/>m mosaic, SCUBA 850 IRAM 1.3 mm we model CB 244 first measured map an entire molecular cloud....
Seven isolated, nearby low-mass starless molecular cloud cores have been observed as part of the Herschel key program Earliest Phases Star formation (EPoS). By applying a ray-tracing technique to obtained continuum emission and complementary (sub)mm maps, we derive physical structure (density, dust temperature) these cores. We present observations 12CO, 13CO, C18O (2-1) N2H+ (1-0) transitions towards same Based on density temperature profiles, apply time-dependent chemical line-radiative...
The mid- and far-infrared view on high-mass star formation, in particular with the results from Herschel space observatory, has shed light many aspects of massive formation. However, these continuum studies lack kinematic information. We study kinematics molecular gas star-forming regions. complemented PACS SPIRE data 16 regions key project EPoS N2H+ line MOPRA Nobeyama 45m telescope. Using full hyperfine structure, we produced column density, velocity, linewidth maps. These were correlated...
We present 450, 850 μm and 1300 images of regions with embedded candidate protostars. Some them are associated HH objects (HH 7-11, 1-2, 147, 111, 108) have been previously identified in the course a survey. Other were taken from IRAS PSC (04239+2436, 04368+2557, 20050+2720, 20386+6751, 22134+5834, 23011+6126). The new mm/submm show detailed structure some which contain compact sources as well extended emission features. inferred fluxes combined data order to derive temperature dust, its...
Context: How do molecular clouds form out of the atomic phase? And what are relative fractions carbon in ionized, and These questions at heart cloud star formation. Methods: Using multiple observatories from Herschel SOFIA to APEX IRAM 30m telescope, we mapped ([CII]@1900GHz, [CI]@492GHz C18O(2-1)@220GHz) high spatial resolution (12"-25") four young massive infrared dark (IRDCs). Results: The three phases were successfully all regions, only one source [CII] line remained a non-detection....
We have mapped the dust continuum emission from molecular cloud covering a region of 28 pc 94 associated with well-known H ii RCW 106 at 1.2 mm using SIMBA on SEST. The observations, having an HPBW 24´´ (0.4 pc), reveal 95 clumps, which about 50% MSX associations and only 20% IRAS associations. Owing to their higher sensitivity colder angular resolution present observations identify new features also show that most sources in this consist multiple peaks. detected millimeter (MMS) include one...
The region of M 17 has been imaged at 10.5 and 20.0 μm with the groundbased infrared camera MANIAC. In addition to a prominent diffuse emission bar (450 3) extending southeast northwest interface between Hii southwestern molecular cloud, mosaic 133 single frames each wavelength revealed 22 compact sources. One these sources is Kleinmann-Wright-Object another was previously identified as ultra-compact 17-UC1. Combining N-band Q-band data near yielded spectral energy distributions that...
We have mapped the R Corona Australis molecular cloud at 1.2 mm with SIMBA on SEST and detected 25 distinct dust emission peaks. While 7 of them coincide positions previously known young stars, 18 are seemingly not associated any stellar object. discuss nature individual sources conclude that there least four small concentrations objects located along filamentary shaped cloud. A comparison C18O data hints depletion molecules in some cores. Our new results yield conflicting arguments about...
<i>Aims. <i/>Our aim is to understand the evolutionary sequence of high-mass star formation from earliest stage starless cores, via cores with embedded low- intermediate-mass objects, finally protostellar objects.<i>Methods. <i/><i>Herschel<i/> far-infrared PACS and SPIRE observations are combined existing data at longer shorter wavelengths characterize spectral physical evolution massive star-forming regions.<i>Results. <i/>The new <i>Herschel<i/> images spectacularly show youngest cold...