A 230 GHz heterodyne receiver array for the IRAM 30 m telescope

Schüster, K.; Boucher, C.; Brunswig, W.; Carter, M.; Chenu, J.-Y.; Foullieux, B.; Greve, A.; John, D.; Lazareff, B.; Vilanova, Santiago; Perrigouard, Alain; Pollet, Jean-Louis; Sievers, A.; Thum, C.; Wiesemeyer, H.

doi:10.1051/0004-6361:20034179

Cited by 91 publications

(92 citation statements)

References 7 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For the observations, we used the heterodyne receiver array (HERA) of the IRAM 30 m (Schuster et al 2004). It consists of 3 × 3 pixels separated by 24 and has two polarizations, which point at the same location on the sky.…”

Section: Observationsmentioning

confidence: 99%

Large scale IRAM 30 m CO-observations in the giant molecular cloud complex W43

Carlhoff

Luong

Schilke

et al. 2013

A&A

View full text Add to dashboard Cite

We aim to fully describe the distribution and location of dense molecular clouds in the giant molecular cloud complex W43. It was previously identified as one of the most massive star-forming regions in our Galaxy. To trace the moderately dense molecular clouds in the W43 region, we initiated W43-HERO, a large program using the IRAM 30 m telescope, which covers a wide dynamic range of scales from 0.3 to 140 pc. We obtained on-the-fly-maps in 13 CO (2-1) and C 18 O (2-1) with a high spectral resolution of 0.1 km s −1 and a spatial resolution of 12 . These maps cover an area of ∼1.5 square degrees and include the two main clouds of W43 and the lower density gas surrounding them. A comparison to Galactic models and previous distance calculations confirms the location of W43 near the tangential point of the Scutum arm at approximately 6 kpc from the Sun. The resulting intensity cubes of the observed region are separated into subcubes, which are centered on single clouds and then analyzed in detail. The optical depth, excitation temperature, and H 2 column density maps are derived out of the 13 CO and C 18 O data. These results are then compared to those derived from Herschel dust maps. The mass of a typical cloud is several 10 4 M while the total mass in the dense molecular gas (>10 2 cm −3 ) in W43 is found to be ∼1.9 × 10 6 M . Probability distribution functions obtained from column density maps derived from molecular line data and Herschel imaging show a log-normal distribution for low column densities and a power-law tail for high densities. A flatter slope for the molecular line data probability distribution function may imply that those selectively show the gravitationally collapsing gas.

show abstract

Section: Observationsmentioning

confidence: 99%

Large scale IRAM 30 m CO-observations in the giant molecular cloud complex W43

Carlhoff

Luong

Schilke

et al. 2013

A&A

View full text Add to dashboard Cite

show abstract

“…In the period between November 2011 and March 2012, we used the 1.3 mm multibeam HEterodyne Receiver Array (HERA) at the IRAM-30 m telescope (Schuster et al 2004) to conduct a CO(2-1) survey of M 31's 0.7 kpc inner ring. One of the fields of this survey contained the center of M 31.…”

Section: Observationsmentioning

confidence: 99%

A cold-gas reservoir to fuel the M 31 nuclear black hole and stellar cluster

Melchior¹,

Combes²

2012

A&A

View full text Add to dashboard Cite

With IRAM-30 m/HERA, we have detected CO(2-1) gas complexes within 30 arcsec (∼100 pc) from the center of M 31 that amount to a minimum total mass of 4.2×10 4 M (one third of the positions are detected). Averaging the whole HERA field, we show that there is no additional undetected diffuse component. Moreover, the gas detection is associated with gas lying on the far side of the M 31 center as no extinction is observed in the optical, but some emission is present on infrared Spitzer maps. The kinematics is complex.(1) The velocity pattern is mainly redshifted: the dynamical center of the gas differs from the black hole position and the maximum of optical emission, and only the redshifted side is seen in our data. (2) Several velocity components are detected in some lines of sight. Our interpretation is supported by the reanalysis of the effect of dust on a complete planetary nebula sample. Two dust components are detected with respective position angles of 37 deg and -66 deg. This is compatible with a scenario where the superposition of the (PA = 37 deg) disk is dominated by the 10 kpc ring and the inner 0.7 kpc ring detected in infrared data, whose position angle (-66 deg) we measured for the first time. The large-scale disk, which dominates the HI data, is steeply inclined (i = 77 deg), warped and superposed on the line of sight on the less inclined inner ring. The detected CO emission might come from both components.

show abstract

“…Images were created with natural weighting and CLEANed using the standard Högbom algorithm. (Schuster et al 2004) at 1 mm with a bandwidth of ∼140 MHz. Sampling at 3 mm was of 15 , while at 1 mm it was of 6 .…”

Section: Observations and Data Reductionmentioning

confidence: 99%

High-angular resolution observations of methanol in the infrared dark cloud core G11.11-0.12P1

Gómez

Wyrowski

Pillai

et al. 2011

A&A

View full text Add to dashboard Cite

Recent studies suggest that infrared dark clouds (IRDCs) have the potential of harboring the earliest stages of massive star formation and indeed evidence for this is found toward distinct regions within them. We present a study with the Plateau de Bure Interferometer of a core in the archetypal filamentary IRDC G11.11-0.12 of a few arcsecond resolution to determine its physical and chemical structures. The data consist of continuum and line observations covering the C 34 S 2 → 1 line and the methanol 2 k → 1 k v t = 0 lines at 3 mm and the methanol 5 k → 4 k v t = 0 lines at 1 mm. Our observations show extended emission in the continuum at 1 and 3 mm. The methanol 2 k → 1 k v t = 0 emission has three maxima extending over a 1 pc scale (when merged with single-dish short-spacing observations); one of the maxima is spatially coincident with the continuum emission. The fitting results show an enhanced methanol fractional abundance (∼3 × 10 −8 ) at the central peak with respect to the other two peaks, where it decreases by about an order of magnitude (∼4−6 × 10 −9 ). Evidence of extended 4.5 μm emission, "wings" in the CH 3 OH 2 k → 1 k spectra, and CH 3 OH abundance enhancements point to the presence of an outflow in the east-west direction. In addition, we find a gradient of ∼4 km s −1 in the same direction, which we interpret as being produced by an outflow(s)-cloud interaction.

show abstract

A 230 GHz heterodyne receiver array for the IRAM 30 m telescope

Cited by 91 publications

References 7 publications

Large scale IRAM 30 m CO-observations in the giant molecular cloud complex W43

Large scale IRAM 30 m CO-observations in the giant molecular cloud complex W43

A cold-gas reservoir to fuel the M 31 nuclear black hole and stellar cluster

High-angular resolution observations of methanol in the infrared dark cloud core G11.11-0.12P1

Contact Info

Product

Resources

About