A Robotic Wide‐Angle Hα Survey of the Southern Sky

By J. Gaustad, P. McCullough, W. Rosing, D. Van Buren. 2001

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We have completed a robotic wide‐angle imaging survey of the southern sky (δ = +15° to −90°) at 656.3 nm wavelength, the Hα emission line of hydrogen. Each image of the resulting Southern Hα Sky Survey Atlas (SHASSA) covers an area of the sky 13° square at an angular resolution of approximately 0.′8 and reaches a sensitivity level of 2 R (1.2 × 10-17 ergs cm−2 s−1 arcsec−2) pixel−1, corresponding to an emission measure of 4 cm−6 pc and to a brightness temperature for microwave free‐free emission of 12 μK at 30 GHz. Smoothing over several pixels allows features as faint as 0.5 R to be detected.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b8f24558bea53045f1d86df0465547a34ac3e123

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Citations in the corpus

The warm ionized medium in spiral galaxies (2009, methodology): “Through CCD imaging, Dennison et al. (1998) has provided partial coverage of the total Hα intensity in the northern sky, while Gaustad et al. (2001) covered the southern sky at arcminute resolution and sensitivities around 1 R (106/4π photons cm−2 s−1 sr−1; EM = 2.25 cm−6 pc at 8000 K).”
A NEW ELECTRON-DENSITY MODEL FOR ESTIMATION OF PULSAR AND FRB DISTANCES (2016, background): “As seen in radio continuum (Hughes et al. 2007) and Hα (Gaustad et al. 2001), 30 Doradus is not far from the nominal center of the LMC at (a30D, )d30D =(05h 40m, - 69 ¢00 ) and it is believed to be at a similar distance.”
Radio observational constraints on Galactic 3D-emission models (2007, background): “…(2003) have constructed an extinction corrected free-free emission template for about 95% of the sky based on Hα surveys of the northern sky (Haffner et al. 2003) and of the southern sky (Gaustad et al. 2001) by using dust emission data (Schlegel et al. 1998) to calculate the extinction correction.”
The Macquarie/AAO/Strasbourg Hα Planetary Nebula Catalogue: MASH (2006, methodology): “We also plan to determine accurate, integrated Hα fluxes for all well resolved MASH PNe using the SHS survey calibration to a Rayleigh scale made possible through direct comparisons with the Southern Hα Sky Survey Atlas (SHASSA) of Gaustad et al. (2001).”
The optical emission nebulae in the vicinity of WR 48 (Θ Mus): true Wolf–Rayet ejecta or unconnected supernova remnant? (2009, background): “…that of Parker, Gull & Kirshner (1979) (which was the basis for the conclusions of Chu & Treffers (1981)) and the arcminute-resolution SHASSA survey Gaustad et al. (2001) we concluded that this could have easily been identified as a single massive H II region from the point of view of these low…”
TASS Mark IV Photometric Survey of the Northern Sky (2006, methodology): “…describe here in some detail the procedure we use to calibrate the positions of objects in our images, since the task is a common one and other astronomers may be able to adapt our software to meet their needs (as the SHASSA (Gaustad et al. 2001) and ACS (Blakeslee et al. 2003) teams already have).”
A Full-Sky Hα Template for Microwave Foreground Prediction (2003, methodology): “SHASSA The complimentary effort in the south is the Southern HAlpha Sky Survey (SHASSA; Gaustad et al. 2001), using a small camera at Cerro Tololo Inter-American Observatory (CTIO).”
The AAO/UKST SuperCOSMOS Hα survey (2005, methodology): “Gaustad et al. (2001) estimate this by comparison with overlapping WHAM data points and interpolating where there are none.”
The pre-launch Planck Sky Model: a model of sky emission at submillimetre to centimetre wavelengths (2012, methodology): “The map of Dickinson et al. (2003) that uses a Hα emission template (a combination of WHAM (Reynolds et al. 1998) and SHASSA (Gaustad et al. 2001) data) corrected for extinction using the E(B − V) map of Schlegel et al. (1998); 2.”
SPITZER SAGE SURVEY OF THE LARGE MAGELLANIC CLOUD. III. STAR FORMATION AND ∼1000 NEW CANDIDATE YOUNG STELLAR OBJECTS (2008, methodology): “The new calibrations from Calzetti et al. (2007) give an SFR of 0.05M yr−1 using the SAGE MIPS24 image, and 0.14 M yr−1 using the Southern H-Alpha Sky Survey Atlas (SHASSA) images (Gaustad et al. 2001).”
Extended Anomalous Foreground Emission in the WMAP Three-Year Data (2007, methodology): “Our template for this foreground is the Hα map, assembled from the VTSS (Dennison et al. 1998), SHASSA (Gaustad et al. 2001), and WHAM (Haffner et al. 2003) surveys by Finkbeiner (2003).”
Microwave Interstellar Medium Emission Observed by the Wilkinson Microwave Anisotropy Probe (2004, methodology): “Free-Free Although warm ionized gas is well traced by H emission in three recent surveys (VTSS, Dennison et al. 1998; SHASSA, Gaustad et al. 2001; WHAM, Haffner et al. 2003) as presented by Finkbeiner (2003) and corrected for dust using the Schlegel et al. (1998; hereafter SFD98) dust map, one must ”
First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Foreground Emission (2003, positive): “High-resolution, large-scale, maps of Hα (hydrogen n=3→2) emission (Dennison et al. 1998; Haffner et al. 2002; Reynolds et al. 2002; Gaustad et al. 2001) can serve as an approximate template for the free-free emission, except in regions of high interstellar dust optical depth, τ > 1, at the Hα…”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: FINAL MAPS AND RESULTS (2012, methodology): “The Finkbeiner map is a composite of the Virginia Tech Spectral line Survey (Dennison et al. 1998), the Southern H-alpha Sky Survey Atlas (Gaustad et al. 2001), and the Wisconsin H alpha Mapper survey (Haffner et al. 2003).”
The XO Project: Searching for Transiting Extrasolar Planet Candidates (2005, methodology): “For each dark-subtracted and flat-fielded image, we use stars to determine the astromet- ric solution and add it to the header (Gaustad et al. 2001).”
Towards a free–free template for CMB foregrounds (2003, background): “The recently published (Gaustad et al. 2001) Southern H Alpha Sky Survey Atlas (SHASSA) covers the southern sky δ 6 +15◦ at an angular resolution of 0.8 arcmin in each 13◦ field.”