The Low-Resolution DRAO Survey of H<scp>i</scp>Emission from the Galactic Plane. II.

Higgs, L. A.; Landecker, T. L.; Asgekar, A.; Davison, O. S.; Rothwell, Timothy A.; Yar-Uyaniker, A.

doi:10.1086/430213

Cited by 11 publications

(21 citation statements)

References 9 publications

(7 reference statements)

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“…Stray radiation has been an issue for Galactic 21-cm science for 50 years (van Woerden et al 1962;Heiles & Wrixon 1976) and many groups have devised methods to suppress or remove it (e.g., Wrixon & Heiles 1972;Kalberla et al 1980;Lockman et al 1986;Hartmann et al 1996;Higgs et al 2005;Kalberla et al 2010). The most accurate methods solve Eq.…”

Section: Stray Radiationmentioning

confidence: 99%

“…We consider here errors in the LAB survey discovered earlier (Higgs et al 2005) and during the course of this work.…”

Section: D2 Errors In the Lab Surveymentioning

confidence: 99%

“…Only where alternative data are available can the above errors be reliably detected and corrected. This alternative is available for only 13 165 of the 257 762 LAB spectra; in 125 of these 13 165 spectra, a total of 141 spurious features were found (including 33 in the regions surveyed by Higgs et al 2005). Most were small, "dips" or "peaks" with a width of about 2 km s −1 superimposed on real features an order of magnitude larger in both width and height.…”

Section: D2 Errors In the Lab Surveymentioning

confidence: 99%

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Accurate galactic 21-cm H I measurements with the NRAO Green Bank Telescope

Boothroyd

Blagrave

Lockman

et al. 2011

A&A

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Aims. We devise a data reduction and calibration system for producing highly-accurate 21-cm H i spectra from the Green Bank Telescope (GBT) of the NRAO. Methods. A theoretical analysis of the all-sky response of the GBT at 21 cm is made, augmented by extensive maps of the far sidelobes. Observations of radio sources and the Moon are made to check the resulting aperture and main beam efficiencies. Results. The all-sky model made for the response of the GBT at 21 cm is used to correct for "stray" 21-cm radiation reaching the receiver through the sidelobes rather than the main beam. This reduces systematic errors in 21-cm measurements by about an order of magnitude, allowing accurate 21-cm H i spectra to be made at about 9 angular resolution with the GBT. At this resolution the procedures discussed here allow for measurement of total integrated Galactic H i line emission, W, with errors of 3 K km s −1 , equivalent to errors in optically thin N HI of 5 × 10 18 cm −2 .

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Section: Stray Radiationmentioning

confidence: 99%

“…We consider here errors in the LAB survey discovered earlier (Higgs et al 2005) and during the course of this work.…”

Section: D2 Errors In the Lab Surveymentioning

confidence: 99%

Section: D2 Errors In the Lab Surveymentioning

confidence: 99%

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Accurate galactic 21-cm H I measurements with the NRAO Green Bank Telescope

Boothroyd

Blagrave

Lockman

et al. 2011

A&A

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“…Single-antenna data are incorporated into the synthesis maps to ensure accurate representation of all structures from the resolution limit up to the largest scales. The low spatial frequency H i data are observed with the DRAO 26-m Telescope (Higgs & Tapping 2000;Higgs et al 2005). Continuum data are derived from the 408-MHz All-Sky survey (Haslam et al 1982), and from the 1.4 GHz Effelsberg survey (Reich et al 1997).…”

Section: Observationsmentioning

confidence: 99%

Two new Perseus arm supernova remnants discovered in the Canadian Galactic Plane Survey

Kothes

Uyanıker

Reid

2005

A&A

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We report the discovery of two new second-quadrant supernova remnants, G96.0+2.0 and G113.0+0.2, in the data of the Canadian Galactic Plane Survey. The two SNRs are residents of the Perseus spiral arm at distances of 4.0 kpc and 3.1 kpc, respectively. The distances were determined kinematically by associating the objects with neutral hydrogen and molecular material. G96.0+2.0 is most likely located at the edge of a large stellar wind bubble with a systemic velocity of about −44 km s −1 . It consists of a relatively bright shell where the shock is encountering the wall of H i and slowly fades away towards the interior of the stellar wind bubble.The visible part of the remnant has a diameter of about 30 pc and a radio spectral index of α ≈ −0.66 (S ∼ ν α ), indicating that it is a shell-type remnant in an early stage of development. The SNR is most likely the remnant of a type Ib/c supernova explosion. G113.0+0.2 is located in an area of confusing thermal emission not far from the radio-bright supernova remnant Cassiopeia A. It has an unusual elongated structure consisting of a long polarized filament and a more complex head structure that is interacting with a small molecular cloud; it resides in a butterfly-shaped H i cavity, probably a stellar wind bubble. It is about 36 pc long and 15 pc wide at a position angle of 70• with the Galactic Plane. A pulsar with a relatively low period derivative, giving it a characteristic age of 10 million years, is located close to the centre of the radio continuum emission at a Perseus arm distance. Whether the pulsar is the result of the same supernova explosion that created G113.0+0.2 or if it was left behind by an earlier supernova that also shaped the stellar wind bubble remains uncertain.

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“…To carry out this process, we observed several positions toward the galactic plane. Then, the obtained HI 21-cm spectra were compared with calibrated spectra of the same galactic positions previously observed (Higgs and Tapping [5]), obtaining in this way a flux calibration factor. The calibration observations were carried out toward four positions:…”

Section: Observations and Data Reductionmentioning

confidence: 99%

The HI Distribution Observed toward a Halo Region of the Milky Way

et al. 2017

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Abstract:We use observations of the neutral atomic hydrogen (HI) 21-cm emission line to study the spatial distribution of the HI gas in a 80 • × 90 • region of the Galaxy halo. The HI column densities in the range of 3-11 × 10 20 cm −2 have been estimated for some of the studied regions. In our map-obtained with a spectral sensitivity of ∼2 K-we do not detect any HI 21-cm emission line above 2σ at Galactic latitudes higher than ∼46 • . This report summarizes our contribution presented at the conference on the origin and evolution of barionic Galaxy halos.

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The Low-Resolution DRAO Survey of HiEmission from the Galactic Plane. II.

Cited by 11 publications

References 9 publications

Accurate galactic 21-cm H I measurements with the NRAO Green Bank Telescope

Accurate galactic 21-cm H I measurements with the NRAO Green Bank Telescope

Two new Perseus arm supernova remnants discovered in the Canadian Galactic Plane Survey

The HI Distribution Observed toward a Halo Region of the Milky Way

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