The MSX Galactic Plane Survey Submillimeter Results

A review is given of information on the galactic-centre region obtained from recent observations of the 21-cm line from neutral hydrogen, the 18-cm group of OH lines, a hydrogen recombination line at 6 cm wavelength, and the continuum emission from ionized hydrogen.Both inward and outward motions are important in this region, in addition to rotation. Several types of observation indicate the presence of material in features inclined to the galactic plane. The relationship between the H and OH concentrations is not yet clear, but a rough picture of the central region can be proposed.

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Southern Hemisphere Seti Survey: Five Years of Project Meta II

International Astronomical Union Colloquium ◽

10.1017/s0252921100015153 ◽

1997 ◽

Vol 161 ◽

pp. 611-621

Author(s):

Guillermo A. Lemarchand ◽

Fernando R. Colomb ◽

E. Eduardo Hurrell ◽

Juan Carlos Olalde

Keyword(s):

Southern Hemisphere ◽

Scattering Theory ◽

Galactic Plane ◽

Narrow Band ◽

Neutral Hydrogen ◽

Sky Survey ◽

Inertial Frames ◽

Interstellar Scattering ◽

Extraterrestrial Origin ◽

Spectral Channels

AbstractProject META II, a full sky survey for artificial narrow-band signals, has been conducted from one of the two 30-m radiotelescopes of the Instituto Argentino de Radioastronomía (IAR). The search was performed near the 1420 Mhz line of neutral hydrogen, using a 8.4 million channels Fourier spectrometer of 0.05 Hz resolution and 400 kHz instantaneous bandwidth. The observing frequency was corrected both for motions with respect to three astronomical inertial frames, and for the effect of Earths rotation, which provides a characteristic changing signature for narrow-band signals of extraterrestrial origin. Among the 2 × 1013spectral channels analyzed, 29 extra-statistical narrow-band events were found, exceeding the average threshold of 1.7 × 10−23Wm−2. The strongest signals that survive culling for terrestrial interference lie in or near the galactic plane. A description of the project META II observing scheme and results is made as well as the possible interpretation of the results using the Cordes-Lazio-Sagan model based in interstellar scattering theory.

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Nobeyama CO Galactic Plane Survey: New Chapter of the Nobeyama 45-m Telescope

EAS Publications Series ◽

10.1051/eas/1575036 ◽

2015 ◽

Vol 75-76 ◽

pp. 193-194 ◽

Cited By ~ 1

Author(s):

T. Minamidani ◽

T. Umemoto ◽

A. Nishimura ◽

M. Matsuo ◽

S. Fujita ◽

...

Keyword(s):

Galactic Plane

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The H.E.S.S. Galactic plane survey poster

10.22323/1.236.0782 ◽

2016 ◽

Author(s):

Axel Donath ◽

Francois Brun ◽

Svenja Carrigan ◽

Ryan Chaves ◽

Christoph Deil ◽

...

Keyword(s):

Galactic Plane

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GASTON: Galactic Star Formation with NIKA2. Evidence for the mass growth of star-forming clumps

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab200 ◽

2021 ◽

Author(s):

A J Rigby ◽

N Peretto ◽

R Adam ◽

P Ade ◽

M Anderson ◽

...

Keyword(s):

Star Formation ◽

Large Scale ◽

Galactic Plane ◽

High Sensitivity ◽

High Mass ◽

Evolutionary Stage ◽

Mass Star ◽

Mass Growth ◽

Star Forming ◽

Compact Source

Abstract Determining the mechanism by which high-mass stars are formed is essential for our understanding of the energy budget and chemical evolution of galaxies. By using the New IRAM KIDs Array 2 (NIKA2) camera on the Institut de Radio Astronomie Millimétrique (IRAM) 30-m telescope, we have conducted high-sensitivity and large-scale mapping of a fraction of the Galactic plane in order to search for signatures of the transition between the high- and low-mass star-forming modes. Here, we present the first results from the Galactic Star Formation with NIKA2 (GASTON) project, a Large Programme at the IRAM 30-m telescope which is mapping ≈2 deg2 of the inner Galactic plane (GP), centred on ℓ = 23${_{.}^{\circ}}$9, b = 0${_{.}^{\circ}}$05, as well as targets in Taurus and Ophiuchus in 1.15 and 2.00 mm continuum wavebands. In this paper we present the first of the GASTON GP data taken, and present initial science results. We conduct an extraction of structures from the 1.15 mm maps using a dendrogram analysis and, by comparison to the compact source catalogues from Herschel survey data, we identify a population of 321 previously-undetected clumps. Approximately 80 per cent of these new clumps are 70 μm-quiet, and may be considered as starless candidates. We find that this new population of clumps are less massive and cooler, on average, than clumps that have already been identified. Further, by classifying the full sample of clumps based upon their infrared-bright fraction – an indicator of evolutionary stage – we find evidence for clump mass growth, supporting models of clump-fed high-mass star formation.

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Polarimetric and photometric observations of CB54, with analysis of four other dark clouds

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab380 ◽

2021 ◽

Vol 503 (4) ◽

pp. 5274-5290

Author(s):

A K Sen ◽

V B Il’in ◽

M S Prokopjeva ◽

R Gupta

Keyword(s):

Magnetic Field ◽

Near Infrared ◽

Galactic Plane ◽

Photometric Data ◽

Dust Particles ◽

Dark Cloud ◽

Dark Clouds ◽

High Polarization ◽

Field Parallel ◽

Photometric Observations

ABSTRACT We present the results of our BVR-band photometric and R-band polarimetric observations of ∼40 stars in the periphery of the dark cloud CB54. From different photometric data, we estimate E(B − V) and E(J − H). After involving data from other sources, we discuss the extinction variations towards CB54. We reveal two main dust layers: a foreground, E(B − V) ≈ 0.1 mag, at ∼200 pc and an extended layer, $E(B-V) \gtrsim 0.3$ mag, at ∼1.5 kpc. CB54 belongs to the latter. Based on these results, we consider the reason for the random polarization map that we have observed for CB54. We find that the foreground is characterized by low polarization ($P \lesssim 0.5$ per cent) and a magnetic field parallel to the Galactic plane. The extended layer shows high polarization (P up to 5–7 per cent). We suggest that the field in this layer is nearly perpendicular to the Galactic plane and both layers are essentially inhomogeneous. This allows us to explain the randomness of polarization vectors around CB54 generally. The data – primarily observed by us in this work for CB54, by A. K. Sen and colleagues in previous works for three dark clouds CB3, CB25 and CB39, and by other authors for a region including the B1 cloud – are analysed to explore any correlation between polarization, the near-infrared, E(J − H), and optical, E(B − V), excesses, and the distance to the background stars. If polarization and extinction are caused by the same set of dust particles, we should expect good correlations. However, we find that, for all the clouds, the correlations are not strong.

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Periastron Observations of the PSR B1259-63/SS 2883 Binary System

Symposium - International Astronomical Union ◽

10.1017/s0074180900055728 ◽

1996 ◽

Vol 165 ◽

pp. 263-269

Author(s):

Simon Johnston

Keyword(s):

Galactic Plane ◽

Radio Spectrum ◽

Wide Frequency Range ◽

Optical Observations ◽

Rotation Measure ◽

Linearly Polarized ◽

Be Star ◽

Frequency Survey ◽

The Magnetic Field

PSR B1259-63 is a 47-millisecond pulsar which was discovered in a high frequency survey of the galactic plane (Johnston et al. 1992a) and was subsequently found to be in a highly eccentric orbit with a main-sequence Be star known as SS 2883 (Johnston et al. 1992b). Radio observations of the pulsar led to a phase connected timing solution which predicted the epoch of periastron to be 1994 January 9 (MJD 49361.2); optical observations of the Be star led to a determination of its mass and of the size of its circumstellar disk (Johnston et al. 1994a): the star is of approximate spectral type B1e, with mass 10 M⊙ and radius 6 R⊙. If this mass is correct and the pulsar has a mass of 1.4 M⊙, then the inclination angle of the plane of the orbit with respect to the sky is 35°. This pulsar has an unusually flat radio spectrum compared to most pulsars, which makes it easily detectable up to 8.4 GHz. The narrow pulse permits dispersion and scattering measurements for studying the ionized plasma in the system. Moreover, the pulses are highly linearly polarized and permit determination of the rotation measure (RM), allowing measurements of the magnetic field along the line of sight. The 3.5-yr orbit of the pulsar around its companion thus provides us with an excellent probe of the stellar wind of the Be star over a wide frequency range.

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Measurements of the 3.3 μm Diffuse Galactic Emission Feature with AROME

Symposium - International Astronomical Union ◽

10.1017/s0074180900240667 ◽

1990 ◽

Vol 139 ◽

pp. 212-213

Author(s):

M. Giard ◽

F. Pajot ◽

J. M. Lamarre ◽

G. Serra

Keyword(s):

Surface Brightness ◽

Galactic Plane ◽

Elevation Angle ◽

Emission Feature ◽

Field Of View ◽

Interstellar Matter ◽

Galactic Emission ◽

Polycyclic Aromatic ◽

Hydrocarbon Molecules ◽

Ir Emission

AROME∗ is a balloon-borne experiment which was built to carry out measurements of IR emission features in the diffuse galactic flux. The field of view is 0.5° and surface brightness gradients are detected through azimuthal scanning at a constant elevation angle. The detection of a feature is done by comparison of the fluxes measured in narrow and wide photometric bands centered on the feature's wavelength. Two flights have been performed (August 1987, October 1988), which detected a 3.3 μm feature in the direction of the galactic plane −6° < b < 6°, 60° > l > −50°. Since this feature is characteristic of aromatic C-H bonds, we assigned it to the emission of transiently heated polycyclic aromatic hydrocarbon molecules (PAHs). With this assumption, AROME measurements show that PAHs are an ubiquitous component of the interstellar matter which contain about 10% of the available cosmic carbon.

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