Publ. Astron. Soc. Aust., 1999, 16, 35–7 .
The HI Parkes Zone of Avoidance Shallow Survey
P. A. Henning1, L. Staveley-Smith2, R. C. Kraan-Korteweg3 and E. M. Sadler4
1 Institute for Astrophysics, University of New Mexico, Albuquerque, NM, 87131, USA [email protected] 2 Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia [email protected] 3 Departamento de Astronomia, Universidad de Guanajuato, Guanajuato, GTO, CP 36000, Mexico [email protected] 4 School of Physics, University of Sydney, NSW 2006, Australia [email protected] Received 1998 November 2, accepted 1999 January 22
Abstract: The HI Parkes Zone of Avoidance Survey is a 21 cm blind search with the multibeam receiver on the 64-m radiotelescope, looking for galaxies hidden behind the southern Milky Way. The rst, shallow (15 mJy rms) phase of the survey has uncovered 107 galaxies, two-thirds of which were previously unknown. The addition of these galaxies to existing extragalactic catalogues allows the connectivity of a very long, thin lament across the Zone of Avoidance within 3500 km s 1 to become evident. No local, hidden, very massive objects were uncovered. With similar results in the north (the Dwingeloo Obscured Galaxies Survey) our census of the most dynamically important HI-rich nearby galaxies is now complete, at least for those objects whose HI pro les are not totally buried in the Galactic HI signal. Tests are being devised to better quantify this remaining ZOA for blind HI searches. The full survey is ongoing, and is expected to produce a catalogue of thousands of objects when it is nished.
Keywords: zone of avoidance—surveys—galaxies: HI—large-scale structure of universe
1 Introduction the Dwingeloo radiotelescope (Henning et al. 1998; The dust and high stellar density of the Milky Way Rivers, Henning & Kraan-Korteweg 1999, this issue obscures up to 25% of the optical extragalactic sky, p. 48). creating a Zone of Avoidance (ZOA). The resulting incomplete coverage of surveys of external galaxies 2 The Shallow Survey leaves open the possibility that dynamically impor- tant structures, or even nearby massive galaxies, 2.1 Observing Strategy remain undiscovered. The HI Parkes ZOA survey covers the southern Careful searches in the optical and infrared wave ZOA (212 l 36 ; |b| 5 ) over the velocity bands can narrow the ZOA (see Kraan-Korteweg range cz = 1200 to 12700 km s 1. The multibeam & Woudt 1999, this issue p. 53) but in the regions receiver is a focal plane array with 13 beams arranged of highest obscuration and infrared confusion, only in a hexagonal grid. The spacing between adjacent radio surveys can nd galaxies. The 21 cm line of beams is about two beamwidths, each beamwidth neutral hydrogen (HI) passes readily through the being 14 arcmin. The survey is comprised of obscuration, so galaxies with su cient HI can be 23 contiguous rectangular elds which are scanned found through detection of their 21 cm emission. Of parallel to the galactic equator. Eventually, each course, this method will miss HI-poor, early-type patch will be observed 25 times, with scans o set by galaxies, and cannot discriminate HI galaxies with about 1 5 arcmin in latitude. The shallow survey redshifts near zero velocity from Galactic HI. discussed here consists of two scans in longitude Here we describe an HI blind survey for galaxies in separated by b = 17 arcmin, resulting in an rms the southern ZOA conducted with the new multibeam noise of about 15 mJy, equivalent to a 5 HI mass 6 2 receiver on the 64-m Parkes telescope. A survey of detection limit of 4 10 dMpc M (for a galaxy HI galaxies in the northern ZOA is underway with with the typical linewidth of 200 km s 1).
᭧Astronomical Society of Australia 1323-3580/99/010035$05.00 36 P. A. Henning et al.
Figure 1—Left panel shows a right ascension–velocity slice to 5000 km s 1 which includes a galaxy discovered by the survey. h m 1 Galactic HI appears as the strong horizontal feature at zero velocity. Note the extragalactic HI signal at 7 18 , 900 km s . Right panel shows a right ascension–declination plane at the velocity of the suspected signal. The galaxy is evident at 7h18m, 9 .
2.2 Data Visualisation of galaxies which might be associated with the Great After calibration, baseline-subtraction, and creation Attractor (but see Juraszek 1999, this issue p. 38). of data cubes, all done with specially developed However, a striking feature becomes apparent with routines based on aips++ (Barnes et al. 1998; Barnes the addition of the ZOA galaxies. An enormous 1998) the data are examined by eye using the visualisa- lament, which crosses the ZOA twice, is clearly tion package Karma (http://www.atnf.csiro.au/karma). evident when these ZOA data are displayed along with The data are rst displayed as right ascension– optically-known galaxies above and below the plane 1 velocity planes, in strips of constant declination. within 3500 km s (Figure 2.) This structure snakes Data cubes are then rotated, and right ascension– over 180 through the southern sky. Taking a mean 1 declination planes are checked for any suspected distance of 30h Mpc, this implies a linear size of 1 1 galaxies (e.g. Figure 1). 100h Mpc, with thickness of 5h Mpc or less. Also, note the relative emptiness of the Local Void. Three hidden galaxies found on a boundary of the Void 3 Galaxies found by the Shallow Survey (l 30 ) lie at 1500 km s 1. Two of these objects The shallow 21-cm survey of the southern ZOA has were also recovered by the Dwingeloo Obscured been completed, and 107 galaxies with peak HI ux Galaxies Survey (Rivers, Henning & Kraan–Korteweg densities 80 mJy have been catalogued. Re ne- 1999). The positions and redshifts of these objects ment of the measurement of their HI characteristics are consistent with their being members of the is ongoing, but the objects seem to be normal cluster at this location proposed by Roman et al. galaxies. However, of three large multibeam ZOA (1998). galaxies imaged in HI with the ATCA, two were Of the 107 objects found, 28 have counterparts seen to break up into complexes of HI suggestive in the NASA/IPAC Extragalactic Database (NED) of tidally-interacting systems (Staveley-Smith et al. with matching positions and redshifts. Optical 1998). Continued follow-up synthesis observations absorption, estimated from the Galactic dust data are planned to investigate the frequency of these of Schlegel, Finkbeiner & Davis (1998), ranges from interacting systems in this purely HI-selected sample. AB = 1 to more than 60 mag at the positions of the Most of the galaxies are within 4000 km s 1, which 107 galaxies, and is patchy over the survey area. is about the redshift limit for detection of normal No objects lying behind more than about 6 mag of spirals of this shallow phase of the survey. As the obscuration have con rmed counterparts in NED, deep survey continues, spirals at higher velocities as expected. will be recovered. The e ective depth of the shallow The shallow multibeam HI survey connects struc- survey is not quite su cient to recover large numbers tures all the way across the ZOA within 3500 km s 1 Zone of Avoidance Shallow Survey 37
40
20
0
-20
GALACTIC LATITUDE -40 350 300 250 GALACTIC LONGITUDE
Figure 2—Galaxies within v 3500 km s 1. The open circles mark galaxies between 500–1500 km s 1, triangles for 1500–2500 km s 1, and dots for those with 2500–3500 km s 1. High latitude data are taken from the literature (LEDA). Also plotted are galaxies from deep optical ZOA surveys (Kraan-Korteweg & Woudt 1999). The galaxies discovered by the multibeam shallow ZOA survey ll in the lowest galactic latitudes, where optical surveys fail.
for the rst time. The ongoing, deep ZOA survey is operated by the Jet Propulsion Laboratory, Cal- will have su cient sensitivity to connect structures tech, under contract with the National Aeronautics at higher redshifts. and Space Administration. We have also made While 14 of the 107 galaxies lie within 1000 km s 1 use of the Lyon–Meudon Extragalactic Database and are therefore fairly nearby, all of the newly- (LEDA), supplied by the LEDA team at the Centre discovered objects have peak HI ux densities an de Recherche Astronomique de Lyon, Observatoire order of magnitude or more lower than the Circinus de Lyon. The research of P.H. is supported by galaxy. Thus, it seems our census of the most NSF Faculty Early Career Development (CAREER) dynamically important, HI-rich nearby galaxies is Program award AST 95-02268. now complete, at least for those objects with velocities o set from Galactic HI. Simulations are References currently being devised to investigate our sensitivity Barnes, D. G. 1998, in ADASS VII, ed. R. Albrecht et al. to HI galaxies whose signals lie within the frequency (San Francisco: ASP), p. 32 range of the Milky Way’s HI. This will be done by Barnes, D. G., Staveley-Smith, L., Ye, T., & Osterloo, T. embedding arti cial HI signals of varying strength, 1998, in ADASS VII, ed. R. Albrecht et al. (San Francisco: width, position, and frequency, into real data cubes. ASP), p. 89 Henning, P. A., Kraan-Korteweg, R. C., Rivers, A. J., Then, an experienced HI galaxy nder (PH) will Loan, A. J., Lahav, O., & Burton, W. B. 1998, AJ, examine the cubes without previous knowledge of 115, 584 the locations of the fake galaxies. In this way, we Juraszek, S. 1999, PASA, 16, 38 hope to quantify better this remaining blind spot Kraan-Korteweg, R. C., & Woudt, P. A. 1999, PASA, 16, 42 Rivers, A. J., Henning, P. A., & Kraan-Kortewg, R. C. of the HI search method. 1999, PASA, 16, 48 Acknowledgments Roman, A. T., Takeuchi, T. T., Nakanishi, K., & Saito, M. 1998, PASJ, 50, 47 We thank HIPASS ZOA collaborators R. D. Ek- Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, ers, A. J. Green, R. F. Haynes, S. Juraszek, 500, 525 M. J. Kesteven, B. S. Koribalski, R. M. Price and Staveley-Smith, L., Juraszek, S., Koribalski, B. S., Ek- ers, R. D., Green, A. J., Haynes, R. F., Henning, P. A., A. Schr oder. This research has made use of the Kesteven, M. J., Kraan-Korteweg, R. C., Price, R. M., NASA/IPAC Extragalactic Database (NED) which & Sadler, E. M. 1998, AJ, 116, 2717