Filler Programs
The following are WIRE "filler programs", which are essentially
equivalent to the HST snapshot programs. When dead time appears in the
WIRE timeline, it gets filled in with "fillers" which are pointed observations
taken from very large target lists. These are potluck observations - it's
impossible to know ahead of time what may get done.
1. Clusters with Giant Gravitational Arcs
These are galaxy clusters with giant arcs which I have preselected for size in order for there to be a chance of spatially resolving the arcs from the cluster members. In each case I have searched NED in a 15' radius to check for any targets that might violate the brightness constraints. Since the arcs themselves have integrated R band magnitudes of around 20, they should be fairly easily detectable. Since they are clusters, they will have the additional science return of providing some measure of the mid-IR luminosity function for cluster members.
Also, lensing by the cluster itself will extend the sensitivity of WIRE to
greater background galaxy depth than one would naively expect. It is possible
that some of these clusters will be specifically targetted.
Name RA (1950) Dec
CL 0024+16 00 24 00.0 16 52 00.0
Abell 370 02 37 20.5 -01 47 57.6
MS 0440+0204 04 40 31.0 02 04 37.0
MS 1006+1202 10 06 06.0 12 02 00.0
MS 1008-1224 10 08 07.3 -12 25 00.0
Abell 2218 16 35 42.0 66 19 00.0
Abell 2219 16 38 54.0 46 47 00.0
MS 1910+6736 19 10 32.3 67 36 24.0
Abell 2390 21 51 12.0 17 26 00.0
CL 2236-04 22 36 59.9 -04 44 36.5
AC 114 22 56 06.0 -35 03 00.0
2. Interacting Galaxies
These are nearby interacting galaxies which can be resolved by WIRE. They are selected to be large enough to be resolvable, and also to be faint enough to image with WIRE (no mean feat!).
These are particularly interesting in that IRAS left open many questions about the specifics of tidally-triggered starburst activity, since IRAS lacked the spatial resolution to resolve even the galaxies from each other, much less the starburst regions.
Most intriguing are the recent ISO results, as well as results from HST/WFPC2, which show that the optically detected starburst is spatially disparate from the source of most of the mid/far-IR flux.
By combining new WIRE observations with pre-existing optical/near-ir/CO imaging and spectroscopy, it will be possible to examine the relationship between
the thinly veiled optical starburst which dominates the morphology of the
galaxy and the deeply embedded starburst which dominates the galaxy energetics.
Name RA DEC
KPG 10 00 24 24 11 18 00
Arp 146 00 04 10 -06 54 49
NGC34 00 08 33 -12 23 10
NGC232 00 40 17 -23 50 02
AM 0043-474 00 43 59 -47 42 13
AM 0052-321 00 52 32 -32 17 48
AM 0106-464 01 06 32 -46 44 32
NGC 520 01 07 20 00 22 15
MCG0204 01 17 22 14 05 53
AM 0117-412 01 17 43 -41 29 53
KPG 53 02 01 05 14 29 04
AM 0205-232 02 05 09 -23 22 12
KPG 59 02 08 33 03 35 30
Arp 145 02 20 00 41 08 35
AM 0223-403 02 23 14 -40 39 07
NGC958 02 28 11 -03 09 32
AM 0230-524 02 30 42 -52 43 31
AM 0313-545 03 13 43 -55 00 15
AM 0316-573 03 16 12 -57 38 18
AM 0354-423 03 54 03 -42 30 44
AM 0413-283 04 13 09 -28 36 30
AM 0453-385 04 53 06 -38 50 49
AM 0545-453 05 45 49 -45 29 48
KPG 127 07 13 00 85 50 00
NGC 2623 08 35 24 25 55 50
KPG 168 08 39 57 14 27 30
MCG0818 09 33 18 48 41 53
Arp 142 09 35 05 03 00 16
Arp 252 09 42 38 -19 29 42
IC563 09 43 44 03 17 26
NGC3110 10 01 32 -06 14 02
KPG 228 10 11 24 03 41 30
IR10173 10 17 22 08 28 41
KPG 234 10 20 46 20 08 04
KPG 236 10 22 24 17 24 00
KPG 249 10 47 05 33 15 00
KPG 255 10 50 48 17 02 30
KPG 257 10 51 51 17 34 30
NGC 3509 11 01 48 05 06 01
UGC6436 11 23 09 14 56 53
KPG 290 11 30 27 53 23 00
KPG 294 11 35 05 48 09 58
NGC 3921 11 48 28 55 21 26
NGC 4038 11 57 23 -18 59 39
KPG 330 12 18 48 11 48 00
IR12224 12 22 29 -06 24 14
KPG 334 12 23 09 18 29 00
KPG 353 12 41 05 11 50 22
NGC 4676 12 43 44 31 00 18
KPG 356 12 50 06 11 32 30
NGC4922 12 59 01 29 34 59
UGC8387 13 18 19 34 23 49
MCG0334 13 19 42 -16 27 56
NGC5135 13 22 56 -29 34 26
NGC5257 13 37 22 01 05 13
KPG 394 13 44 15 44 06 00
KPG 404 13 56 27 37 41 24
Arp 271 14 00 47 -05 49 47
IR15335 15 33 32 -05 13 59
NGC6285 16 57 44 59 00 40
AM 1806-852 18 06 15 -85 25 30
NGC 6621 18 13 09 68 20 53
KPG 548 20 44 50 00 06 58
NGC 7252 22 17 57 -24 55 50
ESO602 22 28 42 -19 17 31
NGC 7469 23 00 44 08 36 18
NGC 7592 23 15 46 -04 41 20
NGC 7674 23 25 24 08 30 14
NGC 7771 23 48 52 19 49 55
KPG 603 23 59 07 23 12 55