A 10-Ghz Radio-Continuum Survey of the Galactic-Plane Region at the Nobeyama Radio Observatory - A Complex Region at l = 22° – 25°

1985 ◽  
pp. 323-324 ◽  
Author(s):  
Y. Sofue ◽  
H. Hirabayashi ◽  
K. Akabane ◽  
M. Inoue ◽  
T. Handa ◽  
...  
Keyword(s):  
Galactic Plane ◽  
Radio Continuum ◽  
Plane Region ◽  
Radio Observatory ◽  
Complex Region ◽  
L 22

scholarly journals A 10-Ghz radio-continuum survey of the Galactic–plane region at the Nobeyama Radio Observatory - A complex region at ℓ = 22° − 25°

1985 ◽  
Vol 106 ◽  
pp. 323-324
Author(s):  
Y. Sofue ◽  
H. Hirabayashi ◽  
K. Akabane ◽  
M. Inoue ◽  
T. Handa ◽  
...  
Keyword(s):  
Galactic Plane ◽  
Extensive Study ◽  
Radio Continuum ◽  
Plane Region ◽  
Radio Observatory ◽  
Complex Region ◽  
Preliminary Results

Preliminary results of a 10-GHz radio-continuum survey of the galactic-plane region using the 45-m telescope at NRO are presented. An extensive study of a complex region at 22° ≦ ℓ ≦ 25°, |b|≳1° has been made.

scholarly journals A 10-GHZ Radio Continuum Survey of the Galactic Plane

1987 ◽  
Vol 115 ◽  
pp. 538-539
Author(s):  
T. Handa ◽  
Y. Sofue ◽  
N. Nakai ◽  
H. Hirabayashi ◽  
K. Akabane ◽  
...  
Keyword(s):  
Galactic Plane ◽  
Noise Temperature ◽  
Radio Continuum ◽  
Beam Size ◽  
Calibration Source ◽  
Polarization Component ◽  
Radio Observatory ◽  
System Noise ◽  
Ngc 7027 ◽  
5 Ghz

A radio continuum survey of the galactic plane has been made with the 45-m telescope of the Nobeyama Radio Observatory at 10.55 GHz, which is the highest frequency among such surveys. The sensitivity of the telescope was Tb/S = 0.47 K/Jy and the HPBW was 2!6, which was a great advantage because of the same beam size of the Bonn 5-GHz survey (Altenhoff et al. 1978). The receiver was a cooled parametric amplifier. The instantaneous bandwidth was 500 MHz, and the system noise temperature was about 100 K. The calibration source was NGC 7027, which was assumed to be 6.6 Jy. One circular polarization component was observed. The observational parameters are summarized in Table I.

scholarly journals The galactic plane region near $\mathsf{\ell=93^\circ}$

2001 ◽  
Vol 367 (2) ◽  
pp. 635-651 ◽  
Author(s):  
T. Foster ◽  
D. Routledge
Keyword(s):  
Galactic Plane ◽  
Plane Region

scholarly journals CO line and radio continuum study of elephant trunks: the Pillars of Creation in M16

2020 ◽  
Vol 492 (4) ◽  
pp. 5966-5979 ◽  
Author(s):  
Yoshiaki Sofue
Keyword(s):  
Surface Brightness ◽  
Galactic Plane ◽  
Brightness Distribution ◽  
Radio Continuum ◽  
Very Large Array ◽  
Heating Source ◽  
Velocity Gradients ◽  
Magnetic Oscillation ◽  
H Ii Region ◽  
Line Survey

ABSTRACT Molecular line and radio continuum properties of the elephant trunks (ET, Pillars of Creation) in M16 are investigated by analysing 12CO(J = 1−0) , 13CO(J = 1−0) and C18O(J = 1−0) line survey data from the Nobeyama 45-m telescope and the Galactic plane radio survey at 20 and 90 cm with the Very Large Array. The head clump of Pillar West I is found to be the brightest radio source in M16, showing a thermal spectrum and the properties of a compact H ii region, with the nearest O5 star in NGC 6611 being the heating source. The radio pillars have a cometary structure concave to the molecular trunk head, and the surface brightness distribution obeys a simple illumination law from a remote excitation source. The molecular density in the pillar head is estimated to be several 104 H2 cm−3 and the molecular mass is $\sim 13\!-\!40 \, \mathrm{M}_\odot$. CO-line kinematics reveals random rotation of the clumps in the pillar tail at ∼1–2 km s−1, comparable with the velocity dispersion and estimated Alfvén velocity. It is suggested that the random directions of the velocity gradients would manifest as torsional magnetic oscillation of the clumps around the pillar axis.

Observations of the large-scale infrared emission from the galactic plane region by the diffuse infrared background experiment

1993 ◽  
Author(s):  
Thomas J. Sodroski ◽  
Richard G. Arendt ◽  
Michael G. Hauser ◽  
Nancy W. Boggess ◽  
Eli Dwek ◽  
...  
Keyword(s):  
Large Scale ◽  
Galactic Plane ◽  
Infrared Emission ◽  
Plane Region ◽  
Infrared Background

scholarly journals Ultracompact H ii regions with extended emission: the complete view

2019 ◽  
Vol 492 (1) ◽  
pp. 895-914 ◽  
Author(s):  
Eduardo de la Fuente ◽  
Alicia Porras ◽  
Miguel A Trinidad ◽  
Stanley E Kurtz ◽  
Simon N Kemp ◽  
...  
Keyword(s):  
Morphological Study ◽  
Galactic Plane ◽  
Radio Continuum ◽  
H Ii Regions ◽  
Direct Connection ◽  
Infrared Excess ◽  
Very Large Array ◽  
Bubble Structure ◽  
Colour Composite ◽  
Extended Emission

ABSTRACT In this paper, we present the results of a morphological study performed on a sample of 28 ultracompact H ii (UC H ii) regions located near extended free–free emission, using radio continuum (RC) observations at 3.6 cm with the C and D Very Large Array (VLA) configurations, with the aim of determining a direct connection between them. By using previously published observations in B and D VLA configurations, we compiled a final catalogue of 21 UC H ii regions directly connected with the surrounding extended emission (EE). The observed morphology of most of the UC H ii regions in RC emission is irregular (single- or multipeaked sources) and resembles a classical bubble structure in the Galactic plane with well-defined cometary arcs. RC images superimposed on colour composite Spitzer images reinforce the assignations of direct connection by the spatial coincidence between the UC components and regions of saturated 24 μm emission. We also find that the presence of EE may be crucial to understand the observed infrared excess because an underestimation of ionizing Lyman photons was considered in previous works (e.g. Wood & Churchwell; Kurtz, Churchwell & Wood).

scholarly journals Distribution of CO in the Southern Milky Way and large-scale structure in the Galaxy

1985 ◽  
Vol 106 ◽  
pp. 203-204
Author(s):  
W.H. Mccutcheon ◽  
B. J. Robinson ◽  
R. N. Manchester ◽  
J. B. Whiteoak
Keyword(s):  
Large Scale ◽  
Milky Way ◽  
Galactic Plane ◽  
Large Scale Structure ◽  
Sampling Interval ◽  
Scale Structure ◽  
Plane Region ◽  
The Galaxy ◽  
Csiro Division

The southern galactic-plane region, in the ranges 294° ≤ 1 ≤ 358°, −0°.075 ≤ b ≤ 0°.075, has been surveyed in the J = 1–0 line of 12CO with a sampling interval of 3′ arc. Observations were made with the 4-metre telescope at the CSIRO Division of Radiophysics in 1980 and 1981. Details of equipment and observing procedure are given in Robinson et al. (1982, 1983); see also McCutcheon et al. (1983).

Hard X-ray survey of the Galactic plane region in Crux: A catalog of sources

2006 ◽  
Vol 32 (3) ◽  
pp. 145-148 ◽  
Author(s):  
M. G. Revnivtsev ◽  
S. Yu. Sazonov ◽  
S. V. Molkov ◽  
A. A. Lutovinov ◽  
E. M. Churazov ◽  
...  
Keyword(s):  
Galactic Plane ◽  
Plane Region ◽  
X Ray

scholarly journals CORNISH: A 5 GHz VLA survey of the Galactic plane

2009 ◽  
Vol 5 (H15) ◽  
pp. 781-781
Author(s):  
Cormac R. Purcell ◽  
Melvin G. Hoare ◽  
Keyword(s):  
Star Formation ◽  
Galactic Plane ◽  
Radio Continuum ◽  
High Mass ◽  
Mass Star ◽  
Multi Wavelength ◽  
Region 10 ◽  
5 Ghz ◽  
Infrared Survey ◽  
Key Questions

AbstractThe CORNISH (Co-Ordinated Radio ‘N’ Infrared Survey for High-mass star formation) project is the radio continuum part of a series of multi-wavelength surveys of the Galactic Plane that focus on the northern GLIMPSE-I region (10° < l <65°, |b| < 1°) observed by the SPITZER satellite in the mid-infrared (Churchwell et al. 2009). CORNISH has delivered a complementary 5 GHz arcsecond resolution, radio-continuum survey to address key questions in high-mass star formation as well as many other areas of astrophysics.

scholarly journals GLOSTAR: Radio Source Catalog I. 28° <  ℓ < 36° and |b| < 1°

2019 ◽  
Vol 627 ◽  
pp. A175 ◽  
Author(s):  
S.-N. X. Medina ◽  
J. S. Urquhart ◽  
S. A. Dzib ◽  
A. Brunthaler ◽  
B. Cotton ◽  
...  
Keyword(s):  
Star Formation ◽  
Software Package ◽  
Large Scale ◽  
Galactic Plane ◽  
Planetary Nebulae ◽  
Radio Continuum ◽  
Spectral Indices ◽  
The Galaxy ◽  
Reported Data ◽  
Cross Matching

Context. Radio continuum surveys of the Galactic plane are an excellent way to identify different source populations such as planetary nebulae, H II regions, and radio stars and characterize their statistical properties. The Global View of Star Formation in the Milky Way (GLOSTAR) survey will study the star formation in the Galactic plane between −2° < ℓ < 85° and |b| < 1° with unprecedented sensitivity in both flux density (∼40 μJy beam−1) and range ofangular scales (∼1".5 to the largest radio structures in the Galaxy). Aims. In this paper we present the first results obtained from a radio continuum map of a 16-square-degree-sized region of the Galactic plane centered on ℓ = 32° and b = 0° (28° < ℓ < 36° and |b| < 1°). This map has a resolution of 18″ and a sensitivity of ∼60−150 μJy beam−1. Methods. We present data acquired in 40 h of observations with the VLA in D-configuration. Two 1 GHz wide sub-bands were observed simultaneously and they were centered at 4.7 and 6.9 GHz. These data were calibrated and imaged using the Obit software package. The source extraction was performed using the BLOBCAT software package and verified through a combination of visual inspection and cross-matching with other radio and mid-infrared surveys. Results. The final catalog consists of 1575 discrete radio sources and 27 large scale structures (including W43 and W44). By cross-matching with other catalogs and calculating the spectral indices (S(ν) ∝ να), we have classified 231 continuum sources as H II regions, 37 as ionization fronts, and 46 as planetary nebulae. The longitude and latitude distribution and negative spectral indices are all consistent with the vast majority of the unclassified sources being extragalactic background sources. Conclusions. We present a catalog of 1575 radio continuum sources and discuss their physical properties, emission nature, and relation to previously reported data. These first GLOSTAR results have increased the number of reliable H II regions in this part of the Galaxy by a factor of four.

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