A high-resolution optical and radio study of Milky Way halo gas

Albert, C. E.; Blades, J. C.; Morton, Donald C.; Lockman, Felix J.; Proulx, Marie-Claude; Ferrarese, Laura

doi:10.1086/191816

Cited by 54 publications

(75 citation statements)

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“…It was detected in Ca ii and Na i absorption toward several stars in M15 (D ¼ 10 kpc ;Cohen 1979;Songaila & York 1980;Kennedy et al 1998;Lehner et al 1999). Intermediate-velocity absorption at the same velocity as cloud g1 was also seen toward the star HD 203664 (D ¼ 4:3 AE 0:4 kpc; Albert et al 1993; Little Ryans et al 1996), which lies 3 west of the main cloud core (see Fig. 8).…”

Section: Blandmentioning

confidence: 89%

Distances to Galactic High‐Velocity Clouds. I. Cohen Stream, Complex GCP, Cloud g1

Wakker

York

Wilhelm

et al. 2008

ApJ

182

198

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The high-and intermediate-velocity interstellar clouds (HVCs/IVCs) are tracers of energetic processes in and around the Milky Way. Clouds with near-solar metallicity about 1 kpc above the disk trace the circulation of material between disk and halo (the Galactic fountain). The Magellanic Stream consists of gas tidally extracted from the SMC, tracing the dark matter potential of the Milky Way. Several other HVCs have low metallicity and appear to trace the continuing accretion of infalling intergalactic gas. These assertions are supported by the metallicities (0

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Section: Blandmentioning

confidence: 89%

Distances to Galactic High‐Velocity Clouds. I. Cohen Stream, Complex GCP, Cloud g1

Wakker

York

Wilhelm

et al. 2008

ApJ

182

198

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“…The interstellar media containing Ti  and Ca  are largely cospatial (see Crinklaw et al 1994;Albert et al 1993), and these refractory ions are observed predominantly in the warm neutral ISM. Welty et al (1996) found the mean upper temperature limit of the clouds in their Ca  survey to be 4100 K, though temperatures as low as a few hundred K were found in many cases.…”

Section: Discussionmentioning

confidence: 99%

The CH$_\mathsf{2}$CN^- molecule: carrier of the $\mathsf{\lambda}$8037 diffuse interstellar band?

Cordiner

Sarre²

2007

A&A

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The hypothesis that the cyanomethyl anion CH 2 CN − is responsible for the relatively narrow diffuse interstellar band (DIB) at 8037.8± 0.15 Å is examined with reference to new observational data. The 0 0 0 absorption band arising from the 1 B 1 −X 1 A transition from the electronic ground state to the first dipole-bound state of the anion is calculated for a rotational temperature of 2.7 K using literature spectroscopic parameters and results in a rotational contour with a peak wavelength of 8037.78 Å. By comparison with diffuse band and atomic line absorption spectra of eight heavily-reddened Galactic sightlines, CH 2 CN − is found to be a plausible carrier of the λ8037 diffuse interstellar band provided the rotational contour is Doppler-broadened with a b parameter between 16 and 33 km s The rotational level populations may be influenced by nuclear spin statistics, resulting in the appearance of additional transitions from K a = 1 of ortho CH 2 CN − near 8025 and 8050 Å that are not seen in currently available interstellar spectra. For CH 2 CN − to be the carrier of the λ8037 diffuse interstellar band, either a) there must be mechanisms that convert CH 2 CN − from the ortho to the para form, or b) the chemistry that forms CH 2 CN − must result in a population of K a levels approaching a Boltzmann distribution near 3 K.

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“…Trial fits including a pile-up model for the other four data sets and for all other jet regions had results consistent with zero piled-up events, although scaling the piled-up fraction by the frame time would lead us to expect a pile-up fraction of about 1% (see frame times in Table 1). As in Marshall et al (2001), we use the hydrogen column density of n H ¼ 1:71 ; 10 20 cm À2 given by Albert et al (1993). We perform fits using two methods.…”

Section: Spectral Fitsmentioning

confidence: 99%

NewChandraObservations of the Jet in 3C 273. I. Softer X‐Ray than Radio Spectra and the X‐Ray Emission Mechanism

Jester

Harris

Marshall

et al. 2006

ApJ

123

167

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The jet in 3C 273 is a high-power quasar jet with radio, optical, and X-ray emission, whose size and brightness allow a detailed study of the emission processes acting in it. We present deep Chandra observations of this jet and analyze the spectral properties of the jet emission from radio through X-rays. We find that the X-ray spectra are significantly softer than the radio spectra in all regions of the bright part of the jet, except for the first bright ''knot A,'' ruling out a model in which the X-ray emission from the entire jet arises from beamed inverse Compton scattering of cosmic microwave background photons in a single-zone jet flow. Within two-zone jet models, we find that a synchrotron origin for the jet's X-rays requires fewer additional assumptions than an inverse Compton model, especially if velocity shear leads to efficient particle acceleration in jet flows.

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A high-resolution optical and radio study of Milky Way halo gas

Cited by 54 publications

References 0 publications

Distances to Galactic High‐Velocity Clouds. I. Cohen Stream, Complex GCP, Cloud g1

Distances to Galactic High‐Velocity Clouds. I. Cohen Stream, Complex GCP, Cloud g1

The CH$_\mathsf{2}$CN^- molecule: carrier of the $\mathsf{\lambda}$8037 diffuse interstellar band?

NewChandraObservations of the Jet in 3C 273. I. Softer X‐Ray than Radio Spectra and the X‐Ray Emission Mechanism

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A high-resolution optical and radio study of Milky Way halo gas

Cited by 54 publications

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Distances to Galactic High‐Velocity Clouds. I. Cohen Stream, Complex GCP, Cloud g1

Distances to Galactic High‐Velocity Clouds. I. Cohen Stream, Complex GCP, Cloud g1

The CH$_\mathsf{2}$CN- molecule: carrier of the $\mathsf{\lambda}$8037 diffuse interstellar band?

NewChandraObservations of the Jet in 3C 273. I. Softer X‐Ray than Radio Spectra and the X‐Ray Emission Mechanism

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Product

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The CH$_\mathsf{2}$CN^- molecule: carrier of the $\mathsf{\lambda}$8037 diffuse interstellar band?