A Blind H [CSC]i[/CSC] Survey for Galaxies in the Zone of Avoidance, 308° ≤ [CLC][ITAL]l[/ITAL][/CLC] ≤ 332°

Juraszek, S.; Staveley‐Smith, L.; Kraan-Korteweg, R. C.; Green, Anne; Ekers, R. D.; Haynes, R. F.; Henning, P. A.; Kesteven, Michael; Koribalski, B. S.; Price, R. M.; Sadler, E. M.; Schröder, A. C.

doi:10.1086/301303

Cited by 25 publications

(34 citation statements)

References 17 publications

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“…The total area of line emission is 1.9 beam areas, or (250 pc) 2 . The H91α + H92α spectrum integrated over the lineemitting region shows a clear line detection with 26 σ significance with centroid at 480 km s −1 , compared to the H I systemic velocity of 449 km s −1 (Juraszek et al 2000). The line FWHM is 260 km s −1 after deconvolving the instrumental velocity resolution of 42 km s −1 .…”

Section: Resultsmentioning

confidence: 89%

Detection of the H92αrecombination line from the starbursts in the Circinus galaxy and NGC 1808

Roy

Goss²,

Anantharamaiah

2008

A&A

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Context. Gas ionized by starburst activity radiates radio recombination lines (RRLs), from which one can derive the plasma conditions and the number of massive stars formed in the burst, free of dust obscuration effects. Aims. We aimed to find detectable RRL emission from additional extragalactic starburst systems and to use the line properties to estimate the properties of the ionized gas. Methods. We conducted a search for RRLs in the nearby extragalactic starburst or Seyfert galaxies NGC 1808, the Circinus galaxy, NGC 4038/9, II Zw 40, NGC 6221, NGC 7552, IRAS 18325-5926, IC 5063, and VV 114. We used the Very Large Array with resolution of 3 to 32 and the Australia Telescope Compact Array with resolution of 10 to search for the RRLs H91α and H92α with rest frequencies of 8.6 GHz and 8.3 GHz. From the new detections we derive conditions in the starburst regions. Results. We detected for the first time RRLs from the starburst nuclei in the Circinus galaxy and NGC 1808. The Circinus galaxy was detected in RRL emission with a line strength integrated over the source of 3.2 mJy, making it the fourth-strongest extragalactic RRL emitter known at this frequency (after NGC 4945, M 82, and NGC 253) and so is suitable for detailed study. The line and continuum emission from the Circinus galaxy can be matched by a model consisting of a collection of 50 to 10 000 H II regions with temperatures of 5000 K, densities of 500 cm −3 to 50 000 cm −3 , and a total effective diameter of 3 pc to 50 pc. The Lyman continuum production rate required to maintain the ionization is 1 × 10 52 s −1 to 3 × 10 53 s −1 , which requires 300 to 9000 O5 stars to be produced in the starburst, inferring a star formation rate of 0.2 M yr −1 to 6 M yr −1 . NGC 1808 was detected in RRL emission at 3.9σ with a line strength of 0.47 mJy at the expected velocity. No radio recombination lines were detected from the other galaxies surveyed to a 3σ limit of 0.3 mJy to 1.4 mJy. Conclusions. We have detected RRLs from two galaxies, adding to the small but growing number of known extragalactic RRL emitters. The Circinus galaxy is strong and especially suited to high-quality follow-up spectroscopic study. We derived conditions and star formation rates in the starbursting regions. Uncertainties can be reduced by future multi-transition studies.

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Section: Resultsmentioning

confidence: 89%

Detection of the H92αrecombination line from the starbursts in the Circinus galaxy and NGC 1808

Roy

Goss²,

Anantharamaiah

2008

A&A

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“…Column 6 gives the 2MASS-ID from the extended source catalogue (Two Micron All Sky Survey team 2003); Col. 7 gives the WKK name and the last column gives other IDs from other catalogues. These are IRAS for the IRAS Point Source Catalog (IRAS PSC; Joint IRAS Science Working Group 1988), PMN for Parkes-MIT-NRAO Radio Survey (Griffith et al 1994), HIZOA for Juraszek et al (2000), HIZSS for the H i Parkes ZoA Shallow Survey (Henning et al 2000), NW04 for Nagayama et al (2004), PKS for the Parkes Catalog of radio sources (Wright & Otrupcek 1990) 4U for the Fourth Uhuru Catalog of X-ray Sources (Forman et al 1978), and 1XMM for the First XMM-Newton Serendipitous Source Catalogue (XMM-Newton Survey Science Centre 2003).…”

Section: Comparison With Other Cataloguesmentioning

confidence: 99%

The highly obscured region around PKS 1343 – 601

Schröder¹,

Mamon

Kraan-Korteweg

et al. 2007

A&A

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The highly obscured radio-bright galaxy PKS 1343 -601 at Galactic coordinates of (l, b) = (309.• 7, +1.• 8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ∼30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al. 1998, ApJ, 500, 525) at face value, the absorption in the optical (A B ) ranges from ∼2 m to over 100 m across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas. The NIR galaxy colours from the 7 aperture were used as a probe to measure total Galactic extinction. A comparison with the IRAS/DIRBE Galactic reddening maps suggests that the IRAS/DIRBE values result in a slight overestimate of the true extinction at such low Galactic latitudes, the inferred extinction from the galaxy colours corresponds to about 87% of the IRAS/DIRBE extinctions. Although this determination still shows quite some scatter, it proves the usefulness of NIR surveys for calibrating the IRAS/DIRBE maps in the extinction range of about 2 m < ∼ A B < ∼ 12 m .

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“…The HI searches for galaxies in the optical Zone of Avoidance carried out by, among others, Henning et al (1998) in the north, and by Henning et al (2000) and Juraszek (2000) in the south, were confined to |b| < 5…”

Section: Systematic Consequences Of Obscuration By H  In the Milky Waymentioning

confidence: 99%

An all–sky study of compact, isolated high–velocity clouds

Heij

Braun²,

Burton

2002

A&A

105

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Abstract.We combine the catalog of compact high-velocity H  clouds extracted by de Heij et al. (2002) from the Leiden/Dwingeloo Survey in the northern hemisphere with the catalog extracted by from the Parkes HIPASS data in the southern hemisphere, and analyze the all-sky properties of the ensemble. Compact high-velocity clouds are a subclass of the general high-velocity cloud phenomenon which are isolated in position and velocity from the extended high-velocity Complexes and Streams down to column densities below 1.5 × 10 18 cm −2 . Objects satisfying these criteria for isolation are found to have a median angular size of less than one degree. We discuss selection effects relevant to the two surveys; in particular the crucial role played by obscuration due to Galactic H . Five principal observables are defined for the CHVC population: (1) the spatial deployment of the objects on the sky, (2) the kinematic distribution, (3) the number distribution of observed H  column densities, (4) the number distribution of angular sizes, and (5) the number distribution of H  linewidth. Two classes of models are considered to reproduce the observed properties. The agreement of models with the data is judged by extracting these same observables from simulations, in a manner consistent with the sensitivities of the observations and explicitly taking account of Galactic obscuration. We show that models in which the CHVCs are the H  counterparts of dark-matter halos evolving in the Local Group potential provide a good match to the observables. The best-fitting populations have a maximum HI mass of 10 7 M , a power-law slope of the HI mass distribution in the range −1.7 to −1.8, and a Gaussian dispersion for their spatial distributions of between 150 and 200 kpc centered on both the Milky Way and M 31. Given its greater mean distance, only a small fraction of the M 31 sub-population is predicted to have been detected in present surveys. An empirical model for an extended Galactic halo distribution for the CHVCs is also considered. While reproducing some aspects of the population, this class of models does not account for some key systematic features of the population.

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A Blind H [CSC]i[/CSC] Survey for Galaxies in the Zone of Avoidance, 308° ≤ [CLC][ITAL]l[/ITAL][/CLC] ≤ 332°

Cited by 25 publications

References 17 publications

Detection of the H92αrecombination line from the starbursts in the Circinus galaxy and NGC 1808

Detection of the H92αrecombination line from the starbursts in the Circinus galaxy and NGC 1808

The highly obscured region around PKS 1343 – 601

An all–sky study of compact, isolated high–velocity clouds

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