The First Galactic Plane Survey at 8.35 and 14.35 GH[CLC]z[/CLC]

Langston, G. I.; Minter, Anthony; D'Addario, Larry R.; Eberhardt, Keri; Koski, K.; Zuber, Julianne

doi:10.1086/301382

Cited by 75 publications

(69 citation statements)

References 8 publications

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“…(J2000) = 06:29:53) of the remnant. We have used the position of the center of the nebula derived by Abdo et al (2010), which is based on the morphology of the nebula, rather than the previous position obtained by Langston et al (2000) which was based on single dish radio measurements and which were biased by the bright rim of the asymmetric remnant. It is interesting to note that there appears to be a region of enhanced radio emission at the position of PSR J1907+0631 which might be from a pulsar wind nebula; further multi-wavelength study is required to confirm this.…”

Section: Psr J1907+0631mentioning

confidence: 99%

Timing of 29 Pulsars Discovered in the Palfa Survey

Lyne¹,

Stappers²,

Bogdanov³

et al. 2017

ApJ

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Section: Psr J1907+0631mentioning

confidence: 99%

Timing of 29 Pulsars Discovered in the Palfa Survey

Lyne¹,

Stappers²,

Bogdanov³

et al. 2017

ApJ

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“…Its flux density has been measured at various wavelengths, and is in the range 5.5−8.5 Jy (Manchester 1969;Altenhoff et al 1970;Reifenstein et al 1970;Griffith et al 1994;Langston et al 2000). Adopting a flux density of 7.0 ± 1.5 Jy, a distance of 1.34 kpc, and using Simpson & Rubin's Eq. (1) (1990), we derive the ionizing photon flux, log (N Lyc ) = 48.04 ± 0.10.…”

Section: Distance and Exciting Starmentioning

confidence: 99%

Triggered star formation on the borders of the Galactic H ii region RCW 120

Zavagno¹,

Pomarès²,

Deharveng³

et al. 2007

A&A

157

256

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Context. To investigate the process of star formation triggered by the expansion of an H ii region, we present a multi-wavelength analysis of the Galactic H ii region RCW 120 and its surroundings. The collect and collapse model predicts that the layer of gas and dust accumulated between the ionization and shock fronts during the expansion of the H ii region collapses and forms dense fragments, giving rise to potential sites of massive-star formation. Aims. The aim of our study is to look for such massive fragments and massive young stars on the borders of RCW 120. Methods. We mapped the RCW 120 region in the cold dust continuum emission at 1.2 mm to search for these fragments. We supplemented this study with the available near-(2MASS) and mid-IR (GLIMPSE) data to locate the IR sources observed towards this region and to analyse their properties. We then compared the observational results with the predictions of Hosokawa & Inutsuka's model (2005, ApJ, 623, 917; 2006, ApJ, 646, 240). Results. At 1.2 mm we detected eight fragments towards this region, five located on its borders. The largest fragment has a mass of about 370 M . Class I and Class II young stellar objects are detected all over the region, with some observed far from the ionization front. This result emphasises the possible importance of distant interactions between the radiation, escaping from the ionized region, and the surrounding medium.

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“…4 (two beamwidth). The integration time per point was 16s resulting in a typical rms noise of ∼0.3 K. Compared to the Gillespie et al (1979) data, our database provides a slight improvement in resolution and an increase in sensitivity (at a velocity resolution similar to the one used by Gillespie et al ) of a factor of 80. ii) New flux density determinations derived from radio continuum surveys carried out at 2.417 GHz 1 (Duncan et al 1995), 5.0 GHz 2 (Haynes et al 1978), and 8.75 and 14.35 GHz 3 (Langston et al 2000), and flux density determinations at other frequencies available in the literature. Figure 2 shows that the strongest CO emission mostly falls in the velocity range from -20 to -10 km s −1 .…”

Section: Databasesmentioning

confidence: 99%

Molecular gas associated with RCW 121 and RCW 122

Arnal

Duronea

Testori

2008

A&A

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Aims. We analyse the distribution of the molecular gas towards the region containing the open cluster Havlen-Moffat 1 (HM 1) the Wolf-Rayet stars WR 87, WR 89, and WR 91, and the star forming regions RCW 121 and RCW 122, with the aim of looking for a possible physical relationship among these objects. Methods. We used the carbon monoxide observations carried out at λ ∼ 2.6 mm with the 4 m NANTEN radiotelescope; new flux density determinations derived from already existing radio continuum surveys at 2. 417, 5, 8.35, and 14.35 GHz; continuum flux density determinations available in the literature; and the Midcourse Space Experiment (MSX) and the Improved Reprocessing of the IRAS Survey (IRIS) databases. Results. Adopting a distance of 5 kpc for RCW 121 and RCW 122, we found a giant molecular cloud (GMC) with a linear extent of ∼100 × 20 pc to be associated with galactic star-forming regions. The total mass of this GMC is of the order of 1.2 × 10 6 solar masses and its mean radial velocity is about -15 km s −1 . Within the GMC there are individual molecular gas concentrations, having total molecular masses in the range from 4.6 × 10 4 M (RCW 122 C) to 2.2 × 10 5 M (RCW 122). The CO profiles observed toward the peak of the molecular concentrations are broad, with typical full-width half-maximum around 6 to 7 km s −1 , and show line asymmetries and/or double-peaked shape that change with the observed position within a given CO concentration. An analysis of the MSX and IRAS databases show that each CO concentration has a strong IR counterpart. The dust temperature of these concentrations range from 46 K (RCW 121) to 76 K (RCW 122 C). Their infrared luminosity are a few times 10 5 L . The new radio continuum flux density determinations are in good agreement with previous determinations at other frequencies, and confirm the thermal nature of RCW 121 and RCW 122. Based on the newly-determined 5 GHz flux density, we found that to power these Hii regions, each of them must harbour a sizable number of O type stars. Under the assumption that all the ionizing stars have a O7 V spectral type, at least ∼8 and ∼4 of these stars would be needed to ionize RCW 122 and RCW 121, respectively.

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The First Galactic Plane Survey at 8.35 and 14.35 GH[CLC]z[/CLC]

Cited by 75 publications

References 8 publications

Timing of 29 Pulsars Discovered in the Palfa Survey

Timing of 29 Pulsars Discovered in the Palfa Survey

Triggered star formation on the borders of the Galactic H ii region RCW 120

Molecular gas associated with RCW 121 and RCW 122

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