Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.naic.edu/alfa/ealfa/papers/2005AAS...20719202M.pdf Äàòà èçìåíåíèÿ: Mon Apr 3 19:26:21 2006 Äàòà èíäåêñèðîâàíèÿ: Sat Dec 22 19:10:56 2007 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: ï ï ï ï ï ï ï ï ï ï ï ï ï

AGES, AUDS, ALFALFA, ZOA
Surveying the extragalactic sky from A to Z


Four different surveys
· ALFALFA - wide angle, shallow survey covering 7000 deg2 · AGES - deeper survey targeting different environments - clusters, groups and voids · AUDS - very deep survey for HI at z > 0.1 · ZOA - survey of the galactic plane - piggybacking on other surveys


HIPASS


ALFALFA


AGES


AUDS


ALFALFA
· Two-pass, meridian drift-scan survey · Three times the volume of HIPASS · Best definition to date of the HI Mass Function (HIMF) · Capable of picking out interesting lowmass objects with high-resolution


AGES
· 24-pass drift survey (300s) · Covers different regions:
­ ­ ­ ­ ­ ­ Virgo Cluster (2 fields) Local Void M33 and the Pisces-Perseus filament Abell 1367 cluster Leo I, NGC 7448 and NGC 3193 groups NGC 6555, NGC 2577, NGC 7332, UGC 2082 and NGC 1156 galaxies.


AGES Precursor Observations
· Targeted the M74 (NGC 628) group · Noise falls as t (to 200s)


AGES Precursor Observations
· Targeted the M74 (NGC 628) group · Noise falls as t (to 200s)


AGES Precursor Observations
· Targeted the M74 (NGC 628) group · Noise falls as t (to 200s) · Detected 5 galaxies in the group


KDG 010

dw0137+1540

UGC 1171

AGES Precursor Observations
· Targeted the M74 (NGC 628) group · Noise falls as t (to 200s) · Detected 5 galaxies in the group
NGC 628 (M74)


AGES Precursor Observations
· · · · Targeted the M74 (NGC 628) group Noise falls as t (to 200s) Detected 5 galaxies in the group Detected 22 objects behind the group


AGES Precursor Observations
· · · · Targeted the M74 (NGC 628) group Noise falls as t (to 200s) Detected 5 galaxies in the group Detected 22 objects behind the group


AGES Precursor Observations
· · · · Targeted the M74 (NGC 628) group Noise falls as t (to 200s) Detected 5 galaxies in the group Detected 22 objects behind the group
­ 8 previously uncatalogued ­ 3 with SDSS redshifts ­ None have previous HI measurements


AGES Initial Results
· Observations began December 2005 targeting the field of NGC 1156 · First coverage (4 passes) completed · One previously uncatalogued galaxy detected so far (3300 km/s)


AGES Initial Results
· Observations began December 2005 targeting the field of NGC 1156 · First coverage (4 passes) completed · One previously uncatalogued galaxy detected so far (3300 km/s)


AGES Initial Results
· Observations began December 2005 targeting the field of NGC 1156 · First coverage (4 passes) completed · One previously uncatalogued galaxy detected so far (3300 km/s) · WBL 091 group seen at 10500 km/s


AGES Initial Results
· Observations began December 2005 targeting the field of NGC 1156 · First coverage (4 passes) completed · One previously uncatalogued galaxy detected so far (3300 km/s) · WBL 091 group seen at 10500 km/s


AUDS
· 40 hours integration time per beam · Covers a small area (0.36 deg2) with most of the volume at high redshift · Sensitive to a few times 108 M at z=0.16 · Will study evolution of gas by determining the HIMF at z>0.1 · Expected to detect 36 gals in no-evolution scenario, 50% more with strong evolution.


AUDS Precursor Observations
· 16 hours integration time per beam


AUDS Precursor Observations
· 16 hours integration time per beam


AUDS Precursor Observations
· 16 hours integration time per beam · 9 certain & 6 possible detections at z>0.1


AUDS Precursor Observations
· 16 hours integration time per beam · 9 certain & 6 possible detections at z>0.1


AUDS Precursor Observations
· 16 hours integration time per beam · 9 certain & 6 possible detections at z>0.1 · Detection rate 2-3 times higher than expect from the HIPASS HIMF · Consistent with strong-evolution scenario, but with low significance · See Freudling et al. poster (187.06)


ZOA
· Commensal survey piggy-backing on Pulsar and Galactic surveys · Will reveal structure behind the Galactic Plane that is inaccessible to the optical


ZOA
· Commensal survey piggy-backing on Pulsar and Galactic surveys · Will reveal structure behind the Galactic Plane that is inaccessible to the optical


ZOA
· Commensal survey piggy-backing on Pulsar and Galactic surveys · Will reveal structure behind the Galactic Plane that is inaccessible to the optical · Galactic surveys give a shallow coverage of a wide area · Pulsar surveys give much deeper coverage


ZOA Initial Results
· Observations started with Galactic surveys in Summer 2005 · First observations covered 38 deg2 near longitude 40º · Reached 6 - 6.5 mJy in 4s integration · Detected 9 galaxies, including 6/8 of Parkes HIZOA galaxies from this region


ZOA Initial Results
· Observations started with Galactic surveys in Summer 2005 · First observations covered 38 deg2 near longitude 40º · Reached 6 - 6.5 mJy in 4s integration · Detected 9 galaxies, including 6/8 of Parkes HIZOA galaxies from this region


ZOA Initial Results
· Intend to map full ZOA in Arecibo sky · Will take ~320 hours to cover the inner galaxy (±10 deg) to this sensitivity · Expect to find ~1000 galaxies · Observations with P-ALFA surveys await the arrival of new correlators · These will be deeper but less well sampled and covering a smaller area


Summary
· The four E-ALFA surveys offer different and complementary ways of exploring the HI content of the Universe. · They will dramatically increase the number of known HI sources. · Will increase our knowledge of the distribution and evolution of galaxies in a way not possible at other wavelengths.