Diagnostics

Deshpande, S. S.; Sharma, Bhanu

doi:10.1007/978-94-011-6976-9_25

Cited by 6 publications

(7 citation statements)

References 101 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Thus optical depth variations would be expected with root-mean-square values of about 0.1. This effect is shown in Figure 2 from Deshpande (2000), based on the -2.75 index for the Cas A Perseus arm data. Most of the objects in this paper and FGDT show H I optical changes which are consistent with this level of variation.…”

Section: +557mentioning

confidence: 85%

“…The power spectra of both Cyg A features are, however, an order of magnitude less intense than the Cas A Perseus Arm feature. Deshpande (2000) suggests that this power law power spectrum with a steeper index of −2.75 can be extrapolated to size scales of 40−−100 AU, a factor of almost 40 relative to the smallest scale in the measured Cas A power spectrum. Thus optical depth variations would be expected with root-mean-square values of about 0.1.…”

Section: +557mentioning

confidence: 89%

“…For 3C 138 the changes in opacity are in the range 0.6−0.8 over a size scale of 50 mas (25 AU at a distance of 500 pc). Deshpande (2000) also suggests that structures observed on small scales should only be observed as gradients in optical depth, since the changes on AU scales are only due to larger scale variations. Our H I optical images toward 3C 147 and 3C 138 clearly show discrete H I structures, not simply gradients.…”

Section: +557mentioning

confidence: 99%

“…Deshpande, Dwarakanath, and Goss (2000) have evaluated the structure observed in H I absorption towards Cas A over a linear scale of 4pc to 0.02 pc. Deshpande (2000) has taken the slope of the power spectrum of fluctuations of α = −2.75 and extrapolated to scales smaller by factors of three orders of magnitude (sizes scales smaller than 100 AU)…”

mentioning

confidence: 99%

See 3 more Smart Citations

The Structure of the Cold Neutral Interstellar Medium on 10–100 AU Scales

Faison

Goss

2001

The Astronomical Journal

View full text Add to dashboard Cite

We have used the Very Long Baseline Array (VLBA) and the Very Large Array (VLA) to image Galactic neutral hydrogen in absorption towards four compact extragalactic radio sources with 10 milliarcsecond resolution. Previous VLBA data by Faison et al (1998) have shown the existence of prominent structures in the direction of the extragalactic source 3C 138 with scale sizes of 10-20 AU with changes in HI optical depth in excess of 0.8 ± 0.1. In this paper we confirm the small scale H I optical depth variations toward 3C 147 suggested earlier at a level up to 20 % ± 5% . The sources 3C 119, 2352+495 and 0831+557 show no significant change in H I optical depth across the sources with one sigma limits of 30%, 50%, and 100%. Of the seven sources recently investigated with the VLBA and VLA , only 3C 138 and 3C 147 show statistically significant variations in HI opacities. Deshpande (2000) have attempted to explain the observed small-scale structure as an extension of the observed power spectrum of structure on parsec size scales. The predictions of Deshpande (2000) are consistent with the VLBA H I data observed in the directions of a number of sources, including 3C 147, but are not consistent with our previous observations of the H I opacity structure toward 3C 138.

show abstract

Section: +557mentioning

confidence: 85%

Section: +557mentioning

confidence: 89%

Section: +557mentioning

confidence: 99%

mentioning

confidence: 99%

See 2 more Smart Citations

The Structure of the Cold Neutral Interstellar Medium on 10–100 AU Scales

Faison

Goss

2001

The Astronomical Journal

View full text Add to dashboard Cite

show abstract

“…As such, the ISM in the Bridge may constitute a textbook turbulent structure: one that is not significantly perturbed by SNe or stellar winds and which conforms well to the expected hierarchical spatial-power cascade (e.g. Kolmogorov 1941;Deshpande 2000).…”

Section: Introductionmentioning

confidence: 89%

Hα Emission from the Magellanic Bridge

Müller¹,

Parker²

2007

Publ. – Astron. Soc. Aust

View full text Add to dashboard Cite

Abstract:We present here a preliminary report and commentary of recently processed observations of Hα emission towards the Magellanic Bridge. These data have been analysed in an attempt to quantify the extent to which the stellar population is capable of reshaping the local ISM. We find that the Hα emission regions are small, weak and sparsely distributed, consistent with a relatively quiescent and inactive ISM where radiative and collisional ionisation is inefficient and sporadic. This suggests that energetic processes at the small scale (i.e. ∼tens of pc) do not dominate the energy balance within the ISM of the Bridge, which therefore hosts a pristine turbulent structure, otherwise inaccessible within our own Galaxy. We find Hα emission that is well correlated with detected 12 CO(1-0) line emission (a proxy for molecular hydrogen), as well as other easily identified ring-like Hi features.

show abstract

Introduction

Deshpande¹

1996

Enzyme Immunoassays

View full text Add to dashboard Cite

Diagnostics

Cited by 6 publications

References 101 publications

The Structure of the Cold Neutral Interstellar Medium on 10–100 AU Scales

The Structure of the Cold Neutral Interstellar Medium on 10–100 AU Scales

Hα Emission from the Magellanic Bridge

Introduction

Contact Info

Product

Resources

About