A ROSAT-detected, New Galactic Supernova Remnant in Sagittarius, G13.3-1.3

Seward, F. D.; Dame, T. M.; Fesen, Robert A.; Aschenbach, B.

doi:10.1086/176089

Cited by 18 publications

(11 citation statements)

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“…13.ÈBeam pattern of the northern telescope, measured in 1994 with a remote transmitter (Dame 1995). The main beam (FWHM) is marked by a white circle.…”

Section: Appendix B Reference Positions (Offs)mentioning

confidence: 99%

“…GMCs are the source of much of the di †use Galactic gamma-ray emission (Hunter et al 1997), and two of the rare gamma-ray repeaters have recently been found to be associated with very massive GMCs (Corbel et al 1997(Corbel et al , 1999. GMCs can be detected in absorption against the di †use X-ray background (Park, Finley, & Dame 1998), and associated supernova remnants are often strong X-ray emitters (e.g., Seward et al 1995 ;Slane et al 1999). If close enough, even quite modest molecular clouds are conspicuous as classical dark nebulae (°3.2), and distant, visually obscured GMCs can be detected as dark nebulae in the near infrared against the Galactic bulge (Kent, Dame, & Fazio 1991).…”

Section: Introductionmentioning

confidence: 99%

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The Milky Way in Molecular Clouds: A New Complete CO Survey

Dame

Hartmann

Thaddeus

2001

ApJ

Self Cite

2,122

178

2,713

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New large-scale CO surveys of the Ðrst and second Galactic quadrants and the nearby molecular cloud complexes in Orion and Taurus, obtained with the CfA 1.2 m telescope, have been combined with 31 other surveys obtained over the past two decades with that instrument and a similar telescope on Cerro Tololo in Chile, to produce a new composite CO survey of the entire Milky Way. The survey consists of 488,000 spectra that Nyquist or beamwidth sample the entire Galactic plane over a (1 8 ¡) strip 4¡È10¡ wide in latitude, and beamwidth or sample nearly all large local clouds at higher lati-1 4 ¡ tudes. Compared with the previous composite CO survey of Dame et al. (1987), the new survey has 16 times more spectra, up to 3.4 times higher angular resolution, and up to 10 times higher sensitivity per unit solid angle. Each of the component surveys was integrated individually using clipping or moment masking to produce composite spatial and longitude-velocity maps of the Galaxy that display nearly all of the statistically signiÐcant emission in each survey but little noise.The composite maps provide detailed information on individual molecular clouds, suggest relationships between clouds and regions widely separated on the sky, and clearly display the main structural features of the molecular Galaxy. In addition, since the gas, dust, and Population I objects associated with molecular clouds contribute to the Galactic emission in every major wavelength band, the precise kinematic information provided by the present survey will form the foundation for many large-scale Galactic studies.A map of molecular column density predicted from complete and unbiased far-infrared and 21 cm surveys of the Galaxy was used both to determine the completeness of the present survey and to extrapolate it to the entire sky at o b o \ 32¡. The close agreement of the observed and predicted maps implies that only D2% of the total CO emission at o b o \ 32¡ lies outside our current sampling, mainly in the regions of Chamaeleon and the Gum Nebula. Taking into account this small amount of unobserved emission, the mean molecular column density decreases from D3 ] 1020 cm~2 at o b o \ 5¡ to D0.1 ] 1020 cm~2 at o b o \ 30¡ ; this drop is D6 times steeper than would be expected from a planeparallel layer, but is consistent with recent measurements of the mean molecular column density at higher latitudes.The ratio of the predicted molecular column density map to the observed CO intensity map provides a calibration of the mass conversion factor Out of the Galactic plane, X shows little systematic variation with latitude from a mean value of (1.8^0.3) ] 1020 cm~2 K~1 km~1 s. Given the large sky area and large quantity of CO data analyzed, we conclude that this is the most reliable measurement to date of the mean X value in the solar neighborhood.

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“…13.ÈBeam pattern of the northern telescope, measured in 1994 with a remote transmitter (Dame 1995). The main beam (FWHM) is marked by a white circle.…”

Section: Appendix B Reference Positions (Offs)mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Milky Way in Molecular Clouds: A New Complete CO Survey

Dame

Hartmann

Thaddeus

2001

ApJ

Self Cite

2,122

178

2,713

View full text Add to dashboard Cite

show abstract

“… References: (1) Sakano et al (2004); (2) Predehl & Truemper (1994); (3) Reynolds et al (2007); (4) Oliva et al (1989); (5) Rho & Petre (1998); (6) Long et al (1991); (7) Seward et al (1995); (8) Saken et al (1995); (9) Lu et al (2002); (10) Koo et al (2008); (11) Hui & Becker (2009); (12) Mavromatakis et al (2001); (13) Li, Lu & Li (2005); (14) Hester & Kulkarni (1989); (15) Katsuda et al (2008); (16) Parker (1967); (17) Durant & van Kerkwijk (2006); (18) Fesen & Hurford (1995); (19) Hwang et al (2004); (20) Hurford & Fesen (1996); (21) Craig, Hailey & Pisarski (1997); (22) Fesen et al (1997); (23) Slane et al (1997); (24) Mavromatakis et al (2000); (25) Warren et al (2005); (26) Ruiz‐Lapuente (2004); (27) Gotthelf, Helfand & Newburgh (2007); (28) Fesen, Kirshner & Becker (1988); (29) Fesen et al (1995); (30) Massaro et al (2006); (31) Sollerman et al (2000); (32) Hui & Becker (2006); (33) Gorenstein (1975); (34) Manzali, De Luca & Caraveo (2007); (35) Manchester et al (1978); (36) De Luca et al (2004); (37) Ruiz (1983); (38) Acero, Ballet & Decourchelle (2007); (39) Raymond, Blair & Long (1995); (40) De Luca et al (2006). …”

Section: Extinction and X‐ray Absorption Measurementsmentioning

confidence: 99%

The relation between optical extinction and hydrogen column density in the Galaxy

Güver

Özel

2009

Monthly Notices of the Royal Astronomical Society

549

221

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A linear relation between the hydrogen column density (N H ) and optical extinction (A V ) in the Galaxy has long been observed. A number of studies found differing results in the slope of this relation. Here, we utilize the data on 22 supernova remnants that have been observed with the latest generation X-ray observatories and for which optical extinction and/or reddening measurements have been performed and find N H (cm −2 ) = (2.21 ± 0.09) × 10 21 A V (mag). We compare our result with the previous studies and assess any systematic uncertainties that may affect these results.

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“…Boumis et al 2002Boumis et al , 2005Mavromatakis et al 2002Mavromatakis et al , 2005, while in the past decade, observations in X-rays have also detected new Galactic SNRs (e.g. Seward et al 1995; see also Green 2006, for a complete catalogue).…”

Section: Introductionmentioning

confidence: 99%

First optical detection of the supernova remnant G 15.1-1.6

Boumis

Alikakos

Christopoulou³

et al. 2008

A&A

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Deep optical CCD images of the supernova remnant G 15.1−1.6 were obtained where filamentary and diffuse emission was discovered. contaminating the supernova remnant's emission to the east. Furthermore, deep long-slit spectra were taken at two bright filaments and also show that the emission originates from shock-heated gas. An [O iii] filamentary structure is also detected farther to the west, but it lies outside the remnant's boundaries and may not be associated to it. The [O iii] flux suggests shock velocities into the interstellar "clouds" ∼100 km s −1 , while the [S ii]λλ 6716/6731 ratio indicates electron densities up to ∼250 cm −3 . Finally, the Hα emission is measured to be between 2 to 7× 10 −16 erg s −1 cm −2 arcsec −2 , while the lower limit to the distance is estimated at 2.2 kpc.

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A ROSAT-detected, New Galactic Supernova Remnant in Sagittarius, G13.3-1.3

Cited by 18 publications

References 0 publications

The Milky Way in Molecular Clouds: A New Complete CO Survey

The Milky Way in Molecular Clouds: A New Complete CO Survey

The relation between optical extinction and hydrogen column density in the Galaxy

First optical detection of the supernova remnant G 15.1-1.6

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