Catalog of CO radial velocities toward galactic H II regions

Blitz, Leo; Fich, M.; Stark, A. A.

doi:10.1086/190795

Cited by 321 publications

(295 citation statements)

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“…Finally, the known H II regions with angular separations from CI Cam less than 5¡ have distances between D0.9 and D9.0 kpc (Blitz, et al 1982 ;Chan & Fich 1995). CI Cam could reasonably lie at any distance up to D9.0 kpc.…”

Section: T He Distance To CI Cammentioning

confidence: 86%

High‐Dispersion Spectroscopy of the X‐Ray Transient RXTE J0421+560 (=CI Camelopardalis) during Outburst

Robinson

Ivans

Welsh

2002

ApJ

116

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We obtained high-dispersion spectroscopy of CI Cam, the optical counterpart of XTE J0421]560, 2 weeks after the peak of its short outburst in 1998 April. The optical counterpart is a supergiant B[e] star that is emitting a two-component wind, a cool, low-velocity wind and a hot, high-velocity wind. The cool wind, which is the source of narrow emission lines of neutral and ionized metals, has a velocity of 32 km s~1 and a temperature near 8000 K. It is dense, roughly spherical, Ðlls the space around the sgB[e] star, and, based on the size of an infrared-emitting dust shell around the system, extends to a radius between 13 and 50 AU. It carries away mass at a high rate, yr~1. The hot wind M 0 [ 10~6 M _ has a velocity in excess of 2500 km s~1 and a temperature of 1.7^0.3 ] 104 K. From an ultraviolet spectrogram of CI Cam obtained in 2000 March with Hubble Space T elescope, we derive a di †erential extinction E(B[V ) \ 0.85^0.05. We show that the distance to CI Cam is greater than 5 kpc. Based on this revised distance, the X-ray luminosity at the peak of the outburst was L (2È25 keV) [ 3.0 ] 1038 ergs s~1, making CI Cam one of the most luminous X-ray transients. The ratio of quiescent luminosity to peak luminosity in the 2È25 keV band isThein the dense circumstellar wind from the sgB[e] star and burrows through the wind, producing little X-ray emission except for rare transient outbursts. This picture, a compact star traveling in a wide orbit through the dense circumstellar envelope of a sgB[e] star, occasionally producing transient X-ray outbursts, makes CI Cam unique among the known X-ray binaries. There is strong circumstantial evidence that the compact object is a black hole, not a neutron star. We speculate that the X-ray outburst was short because the accretion disk around the compact star is fed from a stellar wind and is smaller than disks fed by Roche lobe overÑow.

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Section: T He Distance To CI Cammentioning

confidence: 86%

High‐Dispersion Spectroscopy of the X‐Ray Transient RXTE J0421+560 (=CI Camelopardalis) during Outburst

Robinson

Ivans

Welsh

2002

ApJ

116

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“…The optical nebula list was compiled from: Ber (Bernes 1977), BFS (Blitz et al 1982), BRC (Sugitani et al 1991), Ced (Cederblad 1946), DG (von Dorschner & Gurtler 1963), GGD (Gyulbudaghian et al 1978), GM1- (Gyulbudaghian & Maghakian 1977a), GM2- (Gyulbudaghian & Maghakian 1977b), GM3- (Gyulbudaghian & Maghakian 1977c), Gy1- (Gyulbudaghian 1982a), Gy2- (Gyulbudaghian 1984a), Gy3- (Gyulbudaghian 1984b), Gy82- (Gyulbudaghian 1982b), NS (Neckel & Staude 1984), Parsamian (Parsamian 1965), PP (Parsamian & Petrosian 1979), RNO (Cohen 1980), Sh1- (Sharpless 1953), Sh2- (Sharpless 1959) andvdB-RN (van de Bergh 1966).…”

Section: Search Methodsmentioning

confidence: 99%

New infrared star clusters in the Northern and Equatorial Milky Way with 2MASS

Bica

Dutra

Soares

et al. 2003

A&A

201

216

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Abstract. We carried out a survey of infrared star clusters and stellar groups on the 2MASS J, H and K s all-sky release Atlas in the Northern and Equatorial Milky Way (350The search in this zone complements that in the Southern Milky Way (Dutra et al. 2003a). The method concentrates efforts on the directions of known optical and radio nebulae. The present study provides 167 new infrared clusters, stellar groups and candidates. Combining the two studies for the whole Milky Way, 346 infrared clusters, stellar groups and candidates were discovered, whereas 315 objects were previously known. They constitute an important new sample for future detailed studies.

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“…There is also an interesting H ii region that might be associated with this complex, SH 2-54, from the catalogue of H ii regions in Sharpless (1959). Its radial velocity was measured by Blitz et al (1982) to be 27.6 ± 0.5 km s −1 , much higher than the average velocity of Ser OB2 quoted above, and the distance from the Sun is 2.0 ± 0.2 kpc, which is compatible within errors with the structures discussed above. In summary, region #2, which harbours many young stars and star-forming regions, is undergoing intense formation of new stars, it is at a distance of 1.5-2.0 kpc from the Sun, and has an age of 4-5 Myr.…”

Section: The Origin Of Ls 5039 and Psr J1825−1446mentioning

confidence: 99%

On the origin of LS 5039 and PSR J1825−1446

Moldón

Ribó

Paredes

et al. 2012

A&A

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Context. The gamma-ray binary LS 5039 and the isolated pulsar PSR J1825−1446 were proposed to have been formed in the supernova remnant (SNR) G016.8−01.1. Aims. We aim to obtain the Galactic trajectory of LS 5039 and PSR J1825−1446 to find their origin in the Galaxy, and in particular to check their association with SNR G016.8−01.1 to restrict their age. Methods. By means of radio and optical observations we obtained the proper motion and the space velocity of the sources. Results. The proper motion of PSR J1825−1446 corresponds to a transverse space velocity of 690 km s −1 at a distance of 5 kpc. Its Galactic velocity at different distances is not compatible with the expected Galactic rotation. The velocity and characteristic age of PSR J1825−1446 make it incompatible with SNR G016.8−01.1. There are no clear OB associations or SNRs crossing the past trajectory of PSR J1825−1446. We estimate the age of the pulsar to be 80-245 kyr, which is compatible with its characteristic age. The proper motion of LS 5039 is μ α cos δ = 7.09 and μ δ = −8.82 mas yr −1 . The association of LS 5039 with SNR G016.8−01.1 is unlikely, although we cannot discard it. The system would have had to be formed in the association Ser OB2 (at 2.0 kpc) if the age of the system is 1.0-1.2 Myr, or in the association Sct OB3 (distance 1.5-2 kpc) for an age of 0.1-0.2 Myr. If the system were not formed close to Ser OB2, the pseudo-synchronization of the orbit would be unlikely. Conclusions. PSR J1825−1446 is a high-velocity isolated pulsar ejected from the Galaxy. The distance to LS 5039, which needs to be constrained by future astrometric missions such as Gaia, is a key parameter for restricting its origin and age.

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Catalog of CO radial velocities toward galactic H II regions

Cited by 321 publications

References 0 publications

High‐Dispersion Spectroscopy of the X‐Ray Transient RXTE J0421+560 (=CI Camelopardalis) during Outburst

High‐Dispersion Spectroscopy of the X‐Ray Transient RXTE J0421+560 (=CI Camelopardalis) during Outburst

New infrared star clusters in the Northern and Equatorial Milky Way with 2MASS

On the origin of LS 5039 and PSR J1825−1446

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