Hi Profile Search

Back to AIfA Hi Surveys Server

This interface allows you to extract HI profiles from the EBHIS, GASS, and the LAB survey. The profiles are generated on the fly using a weighted interpolation with a Gaussian kernel.

The effective beamsize includes telescope beam and beam smearing due to interpolation. The beam for the GASS is 14.5 arcmin (64m Parkes telescope), for EBHIS it is 10.8 arcmin (100m Effelsberg telescope), while for the LAB it is 36 arcmin for declinations > -27.5 deg (25m Dwingeloo telescope) and 30 arcmin for declinations < -27.5 deg (30m Villa Elisa telescope).

Due to interpolations the minimum effective FWHM beam is 16 arcmin for the GASS, 12 armin for EBHIS, and 40 arcmin for the LAB for declinations > -27 deg and 35 arcmin for declinations < -27 deg. This implies for the profiles a different FWHM beam if you select an effective beamsize < 36 arcmin. If you want to compare the calculated column densities, the FWHM needs to be taken into account. Expected uncertainties are in each case at a 2-3% level (about 1% scale uncertainty and 1% for uncertainties in the correction for stray radiation). Additional contributions may be due to noise, residual baseline errors, and RFI (causing occasionally scale errors for the LAB). Column densities are calculated for -400 < v < 400 km/s.

Search Position
Coordinate system
Center RA [h m s]/ l [°]
Dec [±° ' "]/ b [°]
Effective beamsize FWHM [°] ( must be < 1° )
Surveys EBHIS (δ > -4°)
GASS III (δ < 1°)

EBHIS is based on observations with the 100-m telescope of the MPIfR (Max-Planck-Institut für Radioastronomie) at Effelsberg. GASS was observed with the Parkes Radio Telescope as part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO.


If you use data products in your research or publications, please reference the following:


HI4PI Collaboration, N. Ben Bekhti, L. Flöer, et al. (2016) A&A, 594, A116 HI4PI: a full-sky H i survey based on EBHIS and GASS


B. Winkel, J. Kerp, L. Flöer, P. M. W. Kalberla, N. Ben Bekhti, R. Keller and D. Lenz, (2016) A&A 585, A41 The Effelsberg-Bonn H i Survey: Milky Way gas


Kalberla, P.M.W. and Haud, U. (2015) A&A 578, A78 (Highlight: Gass: The Parkes Galactic All-Sky Survey. III)

Kalberla, P.M.W., McClure-Griffiths, N.M., Pisano, D. J. Calabretta, M. R., Ford, H. Alyson, Lockman, Felix J., Staveley-Smith, L., Kerp, J., Winkel, B., Murphy, T., Newton-McGee, K. (2010) A&A, 512, A14 (Highlight: Gass: The Parkes Galactic All-Sky Survey. II)

McClure-Griffiths, N. M.; Pisano, D. J.; Calabretta, M. R.; Ford, H. Alyson; Lockman, Felix J.; Staveley-Smith, L.; Kalberla, P. M. W.; Bailin, J.; Dedes, L.; Janowiecki, S , Gibson, B.K., Murpy, T., Newton-McGee, K. (2009) ApJS, 181, 398 (http://adsabs.harvard.edu/abs/2009ApJS..181..398M)

Data from the first data release are available at http://www.atnf.csiro.au/research/GASS/index.html

LAB Survey

When refering to the LAB Survey, please use the following reference:

Kalberla, P.M.W., Burton, W.B., Hartmann, Dap, Arnal, E.M., Bajaja, E., Morras, R., & Pöppel, W.G.L. (2005), A&A, 440, 775 (http://adsabs.harvard.edu/abs/2005A%26A...440..775K)

Depending on the region of the sky being studied, please cite, in addition to the Kalberla et al. (2005) reference, also the appropriate source of the material used:

Observers were Dap Hartmann and W.B. Burton (Leiden University) for the Dwingeloo telescope, and E.M. Arnal, E. Bajaja, J.J. Larrarte, R. Morras, and W.G.L. Pöppel (Argentine Institute for Radio Astronomy) for the Villa Elisa telescope. Correction for stray radiation and combination of the data by P.M.W. Kalberla (Bonn University).

Webinterface created by Peter Kalberla