4. DATA ANALYSIS AND ATLAS PRESENTATION
4.1. Sample Selection
UIT pointings were chosen by the UIT science team and guest observers
with an emphasis on breadth of coverage of galaxy types, likely UV
brightness, low foreground extinction, and a size (typically more than
5' diameter) which takes advantage of the UIT's large field of
view. Given the short duration of the Astro missions and the brief
(
35 minute) periods
during which the spacecraft was in Earth's shadow, it was not possible
to conduct statistically complete surveys or very deep
exposures. Technical difficulties with the Shuttle data display units
often reduced exposure times below requested values. This atlas includes
data from all Astro-1 UIT frames containing identifiable images of
galaxies, excluding fields centered on the Magellanic Clouds, which have
been discussed elsewhere by
Cheng et al. (1992);
Cornett et al.
(1994,
1997);
Hill et al.
(1993a,
1994a,
1995c);
and Parker et al.
(1996,
1998).
Often, galaxies in addition to the intended target are present in the
field. All galaxies which were readily detectable as UV sources on the
selected UIT images are included in this atlas. Identification of
cataloged sources in the UV frames was accomplished by comparing each
image with Digital Sky Survey images obtained using SkyView
(McGlynn, Scollick,
& White 1996),
and searching relevant catalogs using a 20' radius around the central
coordinate of the image. We did not attempt a rigorous selection of very
faint or uncataloged sources. Examples of examination of UIT data frames
for very low surface brightness objects may be found in
O'Neil et al. (1996).
Table 3 lists the objects which were found to be
UV sources in the Astro-1 images. Sources which are both strongly
detected and have an angular diameter exceeding 30" in the MUV are
classified as "Primary" objects. For these we present multiband imagery,
corresponding azimuthally averaged radial surface brightness profiles
and integrated magnitudes. Objects which are either weakly detected or
appear as point sources are classified as "Secondary" objects. For these
we present UV images and integrated quantities.
Table 3. Atlas Galaxy Sample
|
|
| V0
| D
| Dist.
| Scale
| MB0
| RC3
| RSA
|
Object
(1) | Alt. ID
(2) | R.A. (2000)
(3) | Decl. (2000)
(4) | (km s-1)
(5) | (Mpc)
(6) | Ref.
(7) | (pc arcsec-1)
(8) | (mag)
(9) | Type
(10) | Type
(11)
|
|
| Primary Objects
|
|
| NGC 221...
| M32
| 00 42 41.9
| +40 51 55
| -28
| 0.76
| 1
| 3.7
| -15.70
| cE2
| E2
|
| NGC 224...
| M31
| 00 42 44.4
| +41 16 08
| -121
| 0.76
| 1
| 3.7
| -20.37
| SA(s)b
| Sb I -II
|
| NGC 598...
| M33
| 01 33 50.9
| +30 39 37
| -46
| 0.84
| 2
| 4.1
| -18.54
| SA(s)cd
| Sc(s) II-III
|
| NGC 628...
| M74
| 01 36 42.1
| +15 47 11
| 753
| 7.6
| 3
| 36.8
| -19.58
| SA(s)c
| Sc(s) I
|
| NGC 1068...
| M77
| 02 42 40.2
| -00 00 48
| 1144
| 15.3
| 4
| 74.1
| -21.36
| SA(rs)b Sy2
| Sb(rs) II
|
| NGC 1275...
| Pers A
| 03 19 48.5
| +41 30 45
| 5362
| 71.5
| 4
| 347
| -22.38
| cD,pec Sy2
|
|
| NGC 1316...
| Fornax A
| 03 22 41.6
| -37 12 28
| 1674
| 17.0
| 5
| 82
| -21.73
| SAB(s)0,pec
| Sa,pec
|
| NGC 1317...
|
| 03 22 44.7
| -37 06 10
| 1822
| 17.0
| 5
| 82
| -19.24
| SAB(r)a
| Sa
|
| NGC 1399...
|
| 03 38 29.0
| -35 26 58
| 1323
| 17.0
| 5
| 82
| -20.60
| E1,pec
| E1
|
| NGC 1404...
|
| 03 38 51.7
| -35 35 36
| 1805
| 17.0
| 5
| 82
| -20.18
| E1
| E2
|
| NGC 2146...
|
| 06 18 40.1
| +78 21 19
| 1035
| 13.8
| 4
| 66.9
| -19.65
| SB(s)ab,p
| Sb II,pec
|
| NGC 2992...
|
| 09 45 42.1
| -14 19 39
| 2125
| 28.9
| 4
| 140
| -19.43
| Sa,pec Sy2
| Sa (tides)
|
| NGC 2993...
|
| 09 45 48.4
| -14 22 08
| 2224
| 28.9
| 4
| 140
| -19.46
| Sa,p
| Sab (tides)
|
| NGC 3031...
| M81
| 09 55 33.5
| +69 04 00
| 69
| 3.6
| 6
| 17.4
| -20.05
| SA(s)ab
| Sb(r) I-II
|
| NGC 3034...
| M82
| 09 55 54.0
| +69 40 57
| 323
| 3.6
| 6
| 17.4
| -18.61
| I0
| Amorphous
|
| UGC 5336...
| Ho IX
| 09 57 30.0
| +69 02 00
| 154
| 3.6
| 6
| 17.4
| -13.64
| Im
|
|
| UGC 6697...
|
| 11 43 48.7
| +19 58 12
| 6678
| 86
| 7
| 417
| -20.59
| Im
|
|
| NGC 4151...
|
| 12 10 32.4
| +39 24 30
| 1022
| 13.6
| 4
| 66
| -19.17
| SAB(rs)ab Sy1.5
| Sab
|
| NGC 4321...
| M100
| 12 22 55.2
| +15 49 23
| 1540
| 16
| 8
| 77
| -21.03
| SAB(s)bc
| Sc(s) I
|
|
| Secondary Objects
|
|
| Mrk 335...
|
| 00 06 19.5
| +20 12 09
| 7846
| 105
| 4
| 509
|
| S0/a Sy1
|
|
| NGC 891...
|
| 02 22 33.1
| +42 20 48
| 661
| 8.8
| 4
| 42.7
| -19.23
| SA(s)b?
| Sb on edge
|
| NGC 1267...
|
| 03 18 44.9
| +41 28 04
| 5161
| 71.5
| 4
| 347
|
| E+
|
|
| NGC 1268...
|
| 03 18 44.9
| +41 29 18
| 3226
| 43.0
| 4
| 208
|
| SAB(rs)b
|
|
| NGC 1270...
|
| 03 18 58.5
| +41 28 18
| 4973
| 71.5
| 4
| 347
| -20.71
| E
|
|
| NGC 1272...
|
| 03 19 21.3
| +41 29 32
| 4123
| 71.5
| 4
| 347
| -22.11
| E+
|
|
| NGC 1273...
|
| 03 19 27.2
| +41 32 25
| 5453
| 71.5
| 4
| 347
| -20.75
| SA(r)0?
|
|
| UGC 2665...
|
| 03 19 27.4
| +41 38 07
| 7909
| 104
| 4
| 504
|
| Scd?
|
|
| NGC 1277...
|
| 03 19 51.8
| +41 34 25
| 5084
| 71.5
| 4
| 347
| -20.36
| S0+,pec
|
|
| NGC 1278...
|
| 03 19 54.4
| +41 33 50
| 6148
| 71.5
| 4
| 347
| -21.45
| E,pec
|
|
| NGC 1282...
|
| 03 20 12.1
| +41 22 05
| 2294
| 30.6
| 4
| 148
| -19.30
| E
|
|
| NGC 1396...
|
| 03 38 06.3
| -35 26 25
| 771
| 17.0
| 6
| 82
| -16.35
| SAB0-
|
|
| NGC 2551...
|
| 08 24 49.3
| +73 24 46
| 2384
| 32
| 4
| 155
| -19.50
| SA(s)0/a
| Sb(r) I-II
|
| NGC 3837...
|
| 11 43 56.7
| +19 53 42
| 6230
| 86
| 7
| 417
| -20.42
| E
|
|
| MCG3-30-71...
|
| 11 44 01.9
| +19 46 57
| 4886
| 65
| 4
| 315
| -18.52
| Irr
|
|
| NGC 3842...
|
| 11 44 02.0
| +19 57 01
| 6164
| 86
| 7
| 417
| -21.89
| E
|
|
| CGCG 97-114...
|
| 11 44 47.2
| +19 46 22
| 6369
| 86
| 7
| 417
| -19.37
| Irr
|
|
| NGC 4156...
|
| 12 10 49.7
| +39 28 24
| 6782
| 90
| 4
| 436
| -20.81
| SB(rs)b
|
|
| UGC 7188...
|
| 12 11 16.5
| +39 24 08
| 1030
| 13.6
| 4
| 66
|
| SBm
|
|
| NGC 4470...
|
| 12 29 37.9
| +07 49 22
| 2272
| 16
| 8
| 78
| -18.00
| Sa?
|
|
| NGC 4472...
| M49
| 12 29 46.5
| +07 59 58
| 846
| 16
| 8
| 78
| -21.65
| E2
| E1/S01
|
| NGC 4476...
|
| 12 29 58.7
| +12 20 53
| 1873
| 16
| 8
| 78
| -18.11
| SA(r)0-
| E5,pec
|
| NGC 4478...
|
| 12 30 17.4
| +12 19 44
| 1329
| 16
| 8
| 78
| -18.76
| E2
| E2
|
| NGC 4486...
| M87
| 12 30 49.7
| +12 23 24
| 1229
| 16
| 8
| 78
| -21.43
| E0,pec
| E0
|
|
Notes. - Col. (1): Galaxy identification. Col. (2): Alternate
identification. Col. (3): Right ascension of the galaxy centroid taken
from the
RC3,
in units of hours,
minutes, and seconds. Col. (4): Declination of the galaxy centroid
taken from the
RC3,
in units of degrees, arcminutes, and arcseconds. Col. (5): Recession
velocity in km s-1, corrected to the Galactic standard of
rest as presented in the
RC3.
Col. (6): Adopted distance in megaparsecs. Col. (7): Distance
references, given below. Col. (8): Physical scale in parsecs per arcsec
using the distance given in col. 7. Col. (9): Absolute B
magnitude, derived from BT, corrected for
Galactic foreground absorption, using the distance given in
col. 7. Col. (10): Morphological type from the
RC3.
Col. (11): Morphological type from the Revised Shapely Ames Catalog.
|
References for Distance Estimates. - (1)
Freedman 1990,
Freedman & Madore
1990; (2)
Freedman et al. 1991;
(3) Sohn &
Davidage 1996,
Sharina et al. 1996;
(4) distance obtained from recessional velocity listed in col.
(7) and H0 = 75 km s-1 Mpc-1;
(5) Fornax cluster members,
Kohle et al. 1996,
Shaya et al. 1996,
McMillan et
al. 1993; (6)
Freedman et
al. 1994; (7)
D'Onofrio et al. 1997,
Fruscione & Gavazzi
1990,
Godwin & Peach
1982; (8)
Ferrarese et al. 1996.
|
4.2. Treatment of Images
Table 4 summarizes information pertaining to both
the UIT and ground-based images, such as exposure times and image
sources. A footnoted entry in column (4) indicates that multiple images
of adequate quality were obtained for that object. In such a case, the
listed UIT frame number is the best image of the set (e.g., it has the
longer exposure time or optimally shows low surface brightness
structures). Where there are multiple images for a given filter with
comparable exposure times, the images have been registered, scaled, and
co-added to improve the signal-to-noise ratio. Addition of UIT images
for objects which are only marginally detected does not significantly
enhance the detection. In situations for which a short and a long
exposure exist for a particular object, the shorter exposure was used to
replace any saturated pixels in the longer exposure. Saturated pixels in
the UV data (those with E-unit values
1500 in the notation of
Stecher et al. 1997)
were found for a few of the brightest galaxy nuclei (e.g.,
Mrk 335) and
star-forming regions (as found in NGC 598) but were common in the
optical images. Spatial registration of images was accomplished using
field star astrometry obtained from the HST Guide Star Catalog
(Lasker et al. 1990).
Many of the FUV frames did not contain enough bright field stars to
accurately derive an astrometric solution. In such cases, we used either
spacecraft telemetry, uncataloged field stars, or morphological features
of the targets to register and align the images. For Andromeda (NGC 224), a mosaic covering a roughly
1° field of view was constructed
from two different UIT pointings. Image panels for the primary objects
are presented in
Figures 4a -
22a.
Secondary objects are displayed in
Figures 23a -
23b.
Table 4. Ultraviolet-Optical Image
Information
|
Object
(1) | Filter
(2) | texp
(s)
(3) | UIT Frame/Observatory
(4) | Date
(5) | Calibration
Reference
(6)
|
|
| Primary Objects
|
|
| NGC 221...
| B1
| 582.5
| 0485f
| 1990 Dec 9
|
|
| A1
| 583.5
| 0388f
| 1990 Dec 9
|
|
| NGC 224...
| B1
| 384.5
| 0266f
a
| 1990 Dec 7
|
|
| A1 | 330.5
| 0236f
| 1990 Dec 7
|
|
| NGC 598...
| B1
| 424.5
| 0496fa
| 1990 Dec 9
|
|
| A1
| 416.5
| 0402fa
| 1990 Dec 9
|
|
| R
| 120.0
| KPNOa
| 1992 Jan 1
| 1
|
| H | 600.0
| KPNOa
| 1992 Jan 1
| 2
|
| NGC 628...
| B1
| 514.5
| 0172f
| 1990 Dec 6
|
|
| A1
| 530.5
| 0161f
| 1990 Dec 6
|
|
| B
| 600.0
| MLO
| 1991 Oct 8
| 1,3,4
|
| V
| 300.0
| MLO
| 1991 Oct 8
| 1,3,4
|
| R
| 180.0
| MLO
| 1991 Oct 8
| 1,4
|
| H | 900.0
| MLO
| 1991 Oct 8 | 5
|
| NGC 1068...
| B1
| 563.5
| 0411fa
| 1990 Dec 6
|
|
| A1
| 752.5
| 0303fa
| 1990 Dec 6
|
|
| B
| 300.0
| MLO
| 1991 Dec 1
| 1,6
|
| V
| 150.0
| MLOa
| 1993 Nov 7
| 1,6
|
| R
| 60.0
| KPNO
| 1991 Mar 12
| 6
|
| H | 2040.0
| KPNO
| 1991 Mar 12 | 7
|
| NGC 1275...
| B1
| 563.5
| 0464f
| 1990 Dec 9
|
|
| A1
| 564.5
| 0384fa
| 1990 Dec 9
|
|
| B
| 900.0
| KPNO
| 1991 Mar 8
| 1b
|
| V
| 900.0
| KPNO
| 1991 Mar 8
| 1b
|
| R
| 180.0
| KPNO
| 1991 Mar 13
| 1b
|
| NGC 1316...
| B1
| 545.5
| 0533f
| 1990 Dec 10
|
|
| A1
| 545.5
| 0425f
| 1990 Oct 12
|
|
| B
| 300.0
| CTIO
| 1991 Dec 6
| 1
|
| V
| 180.0
| CTIO
| 1991 Dec 6
| 1
|
| R
| 180.0
| CTIO
| 1991 Dec 6
| 1
|
| H
| 600.0
| CTIO
| 1991 Dec 6
| NCc
|
| NGC 1317...
| B1
| 545.5
| 0533f
| 1990 Dec 10
|
|
| A1
| 545.5
| 0425f
| 1990 Oct 12
|
|
| B
| 600.0
| CTIO
| 1991 Dec 10
| 1b
|
| V
| 600.0
| CTIO
| 1991 Dec 10
| 1b
|
| R
| 180.0
| CTIO
| 1991 Dec 6
| 1b
|
| H
| 900.0
| CTIO
| 1991 Dec 11
| 8
|
| NGC 1399...
| B1
| 1454.5
| 0232f
| 1990 Dec 7
|
|
| A1
| 1099.5
| 0216f
| 1990 Dec 7
|
|
| B
| 300.0
| MLO
| 1990 Jul 19
| 1b
|
| V
| 600.0
| MLO
| 1991 Feb 18
| 1,9
|
| R
| 300.0
| MLO
| 1990 Jul 19
| 1,9b
|
| NGC 1404...
| B1
| 1454.5
| 0232f
| 1990 Dec 7
|
|
| A1
| 1099.5
| 0216f
| 1990 Dec 7
|
|
| NGC 2146...
| B5
| 443.5
| 0545fa
| 1990 Dec 10
|
|
| A1
| 442.5
| 0437f
| 1990 Oct 12
|
|
| B
| 300.0
| KPNO
| 1991 Dec 1
| 1
|
| R
| 180.0
| KPNO
| 1991 Dec 1
| 1
|
| H
| 600.0
| KPNO
| 1991 Dec 31
| 7,10
|
| NGC 2992...
| B1
| 256.5
| 0097f
| 1990 Dec 5
|
|
| A1
| 256.5
| 0090f
| 1990 Dec 5
|
|
| B
| 300.0
| KPNO
| 1991 Dec 9
| 1
|
| V
| 600.0
| CTIO
| 1991 Dec 9
| 1
|
| R
| 600.0
| CTIO
| 1991 Dec 9
| 1
|
| H
| 1800.0
| CTIO
| 1991 Dec 9
| 11
|
| NGC 2993...
| B1
| 256.5
| 0097f
| 1990 Dec 5
|
|
| A1
| 256.5
| 0090f
| 1990 Dec 5
|
|
| B
| 300.0
| KPNO
| 1991 Dec 9
| 1
|
| V
| 600.0
| CTIO
| 1991 Dec 9
| 1
|
| R
| 600.0
| CTIO
| 1991 Dec 9
| 1b
|
| H
| 1800.0
| CTIO
| 1991 Dec 9
| 11
|
| NGC 3031...
| B1
| 640.5
| 0556f
| 1990 Dec 10
|
|
| A1
| 639.5
| 0442f
| 1990 Oct 12
|
|
| B
| 600.0
| KPNO
| 1993 Dec 8
| 1
|
| V
| 600.0
| KPNO
| 1991 Mar 8
| 1
|
| R
| 300.0
| KPNOa
| 1990 May 27
| 1
|
| H
| 600.0
| KPNO
| 1991 Apr 13
| 12
|
| NGC 3034...
| B1
| 270.5
| 0204fa
| 1990 Dec 6
|
|
| A1
| 270.5
| 0194f
| 1990 Dec 6
|
|
| B
| 600.0
| MLO
| 1991 Feb 19
| 13
|
| V
| 600.0
| KPNO
| 1991 Mar 9
| 13
|
| R
| 300.0
| MLOa
| 1991 May 12
| 13
|
| H
| 1200.0
| MLO
| 1991 May 12
| 14
|
| UGC 5336...
| B1
| 640.5
| 0556f
| 1990 Dec 10
|
|
| A1
| 639.5
| 0442f
| 1990 Oct 12
|
|
| B
| 600.0
| KPNO
| 1993 Dec 8
| 1b
|
| R
| 300.0
| KPNOa
| 1990 May 27
| 1b
|
| UGC 6697...
| B5
| 529.5
| 0193f
| 1990 Dec 6
|
|
| A1
| 105.5
| 0184f
| 1990 Dec 6
|
|
| B
| 300.0
| KPNO
| 1992 Jan 1
| 1b
|
| R
| 180.0
| KPNO
| 1992 Jan 1
| 1b
|
| NGC 4151...
| B5
| 1199.5
| 0337fa
| 1990 Dec 8
|
|
| A1
| 293.5
| 0295fa
| 1990 Dec 8
|
|
| B
| 300.0
| KPNO
| 1990 Jun 1
| 1b
|
| V
| 600.0
| KPNO | 1991
Mar 8
| 1b
|
| R
| 180.0
| KPNO
| 1990 Jun 1
| 1
|
| H
| 3600.0
| KPNO
| 1991 Mar 8
| NC
|
| NGC 4321...
| B5
| 226.5
| 0166f
| 1990 Dec 6
|
|
| A5
| 226.5
| 0157f
| 1990 Dec 6
|
|
| B
| 600.0
| KPNO
| 1991 Mar 12
| 1,15
|
| V
| 300.0
| KPNO
| 1991 Mar 12
| 1,15
|
| R
| 180.0
| KPNO
| 1992 Jan 2
| 1,15
|
| H
| 600.0
| KPNO
| 1992 Jan 2
| 16
|
|
| Secondary Objects
|
|
| Mrk 335...
| B1
| 286.5
| 0507fa
| 1990 Dec 10
|
|
| A1
| 294.5
| 0410fa
| 1990 Dec 10
|
|
| NGC 891...
| B5
| 437.5
| 0358fa
| 1990 Dec 8
|
|
| A1
| 437.5
| 0307f
| 1990 Dec 8
|
|
| R
| 300.0
| MLO
| 1992 Aug 23
| NC
|
| H
| 600.0
| MLO
| 1993 Dec 6
| 10
|
| NGC 1267...
| B1
| 563.5
| 0464f
| 1990 Dec 9
|
|
| A1
| 564.5
| 0384fa
| 1990 Dec 9
|
|
| NGC 1268...
| B1
| 563.5
| 0464f
| 1990 Dec 9
|
|
| A1
| 564.5
| 0384fa
| 1990 Dec 9
|
|
| NGC 1270...
| B1
| 563.5
| 0464f
| 1990 Dec 9
|
|
| A1
| 564.5
| 0384fa
| 1990 Dec 9
|
|
| B
| 900.0
| KPNO
| 1991 Mar 8
| 1
|
| V
| 900.0
| KPNO
| 1991 Mar 8
| 1
|
| R
| 180.0
| KPNO
| 1991 Mar 13
| 1b
|
| NGC 1272...
| B1
| 563.5
| 0464f
| 1990 Dec 9
|
|
| A1
| 564.5
| 0384fa
| 1990 Dec 9
|
|
| B
| 900.0
| KPNO
| 1991 Mar 8
| 1
|
| V
| 900.0
| KPNO
| 1991 Mar 8
| 1b
|
| R
| 180.0
| KPNO
| 1991 Mar 13
| 1b
|
| NGC 1273...
| B1
| 563.5
| 0464f
| 1990 Dec 9
|
|
| A1
| 564.5
| 0384fa
| 1990 Dec 9
|
|
| B
| 900.0
| KPNO
| 1991 Mar 8
| 1
|
| V
| 900.0
| KPNO
| 1991 Mar 8
| 1
|
| R
| 180.0
| KPNO
| 1991 Mar 13
| 1b
|
| UGC 2665...
| B1
| 563.5
| 0464f
| 1990 Dec 9
|
|
| A1
| 564.5
| 0384fa
| 1990 Dec 9
|
|
| B
| 900.0
| KPNO
| 1991 Mar 8
| 1b
|
| V
| 900.0
| KPNO
| 1991 Mar 8
| 1b
|
| NGC 1277...
| B1
| 563.5
| 0464f
| 1990 Dec 9
|
|
| A1
| 564.5
| 0384fa
| 1990 Dec 9
|
|
| B
| 900.0
| KPNO
| 1991 Mar 8
| 1
|
| V
| 900.0
| KPNO
| 1991 Mar 8
| 1
|
| R
| 180.0
| KPNO
| 1991 Mar 13
| 1b
|
| NGC 1278...
| B1
| 563.5
| 0464f
| 1990 Dec 9
|
|
| A1
| 564.5
| 0384fa
| 1990 Dec 9
|
|
| B
| 900.0
| KPNO
| 1991 Mar 8
| 1
|
| V
| 900.0
| KPNO
| 1991 Mar 8
| 1
|
| R
| 180.0
| KPNO | 1991
Mar 13
| 1b
|
| NGC 1282...
| B1
| 563.5
| 0464f
| 1990 Dec 9
|
|
| A1
| 564.5
| 0384fa
| 1990 Dec 9
|
|
| B
| 900.0
| KPNO
| 1991 Mar 8
| 1
|
| V
| 900.0
| KPNO
| 1991 Mar 8
| 1
|
| R
| 180.0
| KPNO
| 1991 Mar 13
| 1
|
| NGC 1396...
| B1
| 1454.5
| 0232f
| 1990 Dec 7
|
|
| A1
| 1099.5
| 0216f
| 1990 Dec 7
|
|
| NGC 2551...
| B1
| 454.5
| 0451fa
| 1990 Dec 9
|
|
| A1
| 454.5
| 0380f
| 1990 Dec 9
|
|
| NGC 3837...
| B5
| 529.5
| 0193f
| 1990 Dec 6
|
|
| A1
| 105.5
| 0184f
| 1990 Dec 6
|
|
| B
| 300.0
| KPNO
| 1992 Jan 1
| 1
|
| R
| 180.0
| KPNO
| 1992 Jan 1 | 1b
|
| MCG 3 30 71...
| B5
| 529.5
| 0193f
| 1990 Dec 6
|
|
| A1
| 105.5
| 0184f
| 1990 Dec 6
|
|
| B
| 300.0
| KPNO
| 1992 Jan 1
| 1b
|
| R
| 180.0
| KPNO
| 1992 Jan 1
| 1b
|
| NGC 3842...
| B5
| 529.5
| 0193f
| 1990 Dec 6
|
|
| A1
| 105.5
| 0184f
| 1990 Dec 6
|
|
| B
| 300.0
| KPNO
| 1992 Jan 1
| 1
|
| R
| 180.0
| KPNO
| 1992 Jan 1
| 1b
|
| CGCG 97 114...
| B5
| 529.5
| 0193f
| 1990 Dec 6
|
|
| A1
| 105.5
| 0184f
| 1990 Dec 6
|
|
| NGC 4156...
| B5
| 1199.5
| 0337fa
| 1990 Dec 8
|
|
| A1
| 293.5
| 0295fa
| 1990 Dec 8
|
|
| B
| 300.0
| KPNO
| 1990 Jun 1 | 1
|
| V
| 600.0
| KPNO
| 1991 Mar 8 | 1
|
| R
| 180.0
| KPNO
| 1990 Jun 1
| 1b
|
| H
| 3600.0
| KPNO
| 1991 Mar 8
| NC
|
| UGC 7188...
| B5
| 1199.5
| 0337fa
| 1990 Dec 8
|
|
| A1
| 293.5
| 0295fa
| 1990 Dec 8
|
|
| B
| 300.0
| KPNO
| 1990 Jun 1
| 1b
|
| V
| 600.0
| KPNO
| 1991 Mar 8
| 1b
|
| R
| 180.0
| KPNO
| 1990 Jun 1
| 1b
|
| H
| 3600.0
| KPNO
| 1991 Mar 8
| NC
|
| NGC 4470...
| B5
| 180.5
| 0415f
| 1990 Dec 9
|
|
| A5
| 180.5
| 0338f
| 1990 Dec 9
|
|
| NGC 4472...
| B5
| 180.5
| 0415f
| 1990 Dec 9
|
|
| A5
| 180.5
| 0338f
| 1990 Dec 9
|
|
| NGC 4476...
| B5
| 352.5
| 0125f
| 1990 Dec 5
|
|
| A1
| 70.5
| 0113f
| 1990 Dec 5
|
|
| NGC 4478...
| B5
| 352.5
| 0125f
| 1990 Dec 5
|
|
| A1
| 70.5
| 0113f
| 1990 Dec 5
|
|
| NGC 4486...
| B5
| 352.5
| 0125f
| 1990 Dec 5
|
|
| A1
| 70.5
| 0113f
| 1990 Dec 5
|
|
| B
| 300.0
| MLO
| 1991 Feb 4
| 1,17,18,19
|
| V
| 300.0
| MLO
| 1991 Nov 5
| 1,17,18,19,20
|
| R
| 300.0
| MLOa
| 1991 Nov 5
| 1,21,22
|
|
Notes. - Col. (1): Galaxy identification.
Col. (2): Filter used for this observation.
Col. (3): Exposure time in seconds.
Col. (4): For UIT data this column lists the assigned UIT image frame
number from which the photometry was derived (See
Section 4.2
for details). These frame numbers can be used to access the UIT data
from the HST multimission archive. For optical band imagery,
this column lists the source of the data.
Col. (5): Date of observation.
Col. (6): Literature reference to the published data that was used to
bootstrap the calibration of the optical photometry presented in this
paper.
a Indicates images which have
been co-added with other exposures of the same
target.
b Due to lack of reliable
data, this galaxy was calibrated based on an
average of other galaxies in the field. (See
Section 4.6 for discussion).
c Data are not
calibrated.
References. -(1)
Prugniel &
Heraudeau 1998; (2)
using spectrophotometric standard star Feige 34
(Stone 1977) ; (3)
Frogel 1985; (4)
Elmegreen 1980; (5)
Kennicutt & Hodge
1980; (6)
Schild et
al. 1985; (7)
Young et al. 1988;
(8)
Crocker et
al. 1996; (9)
Mackie et
al. 1990; (10)
Smith & Harvey
1996; (11)
Usui et al. 1998;
(12)
Hill et al. 1995a;
(13) using standard star field; (14)
O'Connell &
Mangano 1978;
(15) de Jong & van
der Kruit 1994,
with applied systematic offsets given by
Prugniel &
Heraudeau 1998; (16)
Kennicutt & Kent
1983; (17)
Goudfrooij et al. 1994,
with applied systematic offsets given by
Prugniel
& Heraudeau 1998; (18)
Michard 1982,
with applied systematic offsets given by
Prugniel &
Heraudeau 1998; (19)
Poulain 1983, private communication, with applied systematic offsets
given by
Prugniel & Heraudeau
1998; (20)
Aaronson & Mould
1981, with applied systematic offsets given by
Prugniel &
Heraudeau 1998; (21)
Djorgovski 1985,
with applied systematic offsets given by
Prugniel &
Heraudeau 1998; (22)
Peletier et
al. 1990, with applied systematic offsets given by
Prugniel &
Heraudeau 1998
| |
|
|
Figure 5. (a) Upper panel:
FUV mosaic of NGC 224 (M31). Lower panel: UV and R-band
(from
Kent 1987)
extinction-corrected radial surface brightness profiles. Note that
offsets (given in the legend) have been applied. (b) Upper
panel: MUV mosaic of NGC 224. Lower panel: UV and
R-band extinction-corrected color profiles. Note that offsets
(given in the legend) have been applied.
|
|
|
Figure 9. (a) UV and optical images
for NGC 1275. (b) UV/optical extinction-corrected
radial surface
brightness (upper) and color (lower) profiles for
NGC 1275. Note that offsets (given in the legend)
have been applied.
|
|
|
Figure 12. (a) UV and optical images
for NGC 1399. (b) UV/optical extinction-corrected
radial surface
brightness (upper) and color (lower) profiles for
NGC 1399. Note that offsets (given in the legend)
have been applied.
|
|
|
Figure 13. (a) UV images for
NGC 1404. (b) UV/optical extinction-corrected
radial surface
brightness (upper) and color (lower) profiles for
NGC 1404.
|
|
|
Figure 14. (a) UV and optical images
for NGC 2146. (b) UV/optical extinction-corrected
radial surface
brightness (upper) and color (lower) profiles for
NGC 2146. Note that offsets (given in the legend)
have been applied.
|
|
|
Figure 17. (a) UV and optical images
for NGC 3031 (M81). (b) UV/optical
extinction-corrected radial
surface brightness (upper) and color (lower) profiles for
NGC 3031.
|
|
|
Figure 19. (a) UV and optical images
for UGC 5336. (b) UV/optical extinction-corrected
radial surface
brightness (upper) and color (lower) profiles for
UGC 5336. Note that offsets (given in the legend)
have been applied.
|
|
|
Figure 20. (a) UV and optical images
for UGC 6697. (b) UV/optical extinction-corrected
radial surface
brightness (upper) and color (lower) profiles for
UGC 6697. Note that offsets (given in the legend)
have been applied.
|
|
|
Figure 23. UV and optical (where available)
images for "secondary" objects.
|
Some Astro-1 images were affected by thin (a few pixels) linear
scratches, apparently on the emulsion surface, which occurred during the
digitalization process. These artifacts have been treated by replacing
the affected pixels with values determined by linear interpolation from
neighboring pixels. Astro-2 images (see
Kuchinski et al. 2000)
are not similarly affected.
4.3. Flux Calibration and Error Analysis
UIT noise characteristics have been determined from repeated
measurements of the pixel values in laboratory flat fields (see
Stecher et al. 1997
for full details). The resulting noise/signal ratio is relatively small
(15%-20% for single pixels and 5% for regions several arcseconds in
size) over the center of the dynamic range, with substantial increases
(
40%) at the extremes. The
photometric uncertainties reported in the tables here combine the
estimated variances for all pixels in a given measuring aperture in
quadrature, treating source pixels and sky as independent contributors
to uncertainty in the flux values.
Absolute flux calibration of UIT was determined by comparing photometry
of stars from selected UIT frames with photometry from IUE, HUT,
ANS, GHRS, and other UV instruments. The primary calibration is based on
isolated stars observed in common with IUE. Typical uncertainties
in absolute fluxes for UIT sources with good exposure were determined to
be ~ 15%
(Stecher et al. 1997).
The majority of the ground-based images were taken under nonphotometric
sky conditions. Broadband optical images in the BVR bands were
calibrated by comparison to a compilation of published aperture and CCD
photometry as given by
Prugniel &
Heraudeau (1998).
All R-band data given in this atlas are based on the Cousins
R
(Bessell 1986)
photometric system. Additional sources were used to flux calibrate the
H and some R-band
images. For the broadband data, calibration scaling factors were derived
from the mean offset (in magnitudes) between all available photometry
and instrumental values determined for matching apertures. Offsets
obtained in this manner inherently account for air mass corrections,
color terms (for that particular object), and instrumental
corrections. We note that foreground stars were masked out during
computation of the photometry presented in this paper. To derive a
calibration by comparison to published values, instrumental magnitudes
were computed without masking foreground stars, on the assumption that
the literature values were derived in this manner. References and
methods used to calibrate the optical data are given in column (6) of
Table 4. Uncalibrated data are indicated as "NC"
in the table.
Continuum-free H images were
obtained by subtracting a scaled R-band image from a narrowband
image centered on
H. Unsaturated stars common
to both images were used to determine the scaling factor applied to the
R-band image. Published
H aperture photometry was
then used to derive an absolute calibration for the pure emission line
image. The narrowband filters used for the
H data presented in the
atlas included possible [N II] emission; no correction has been applied
for this. However, most of the references used to determine absolute
calibrations also included [N II], so the calibrations should be
consistent.
H fluxes are given in units
of ergs s-1 cm-2.
The optical photometry presented here has typical
uncertainties of 0.05 mag. The
H data have a somewhat
larger uncertainty (~ 10%-30%), due to the limited published photometry
available for calibration and to uncertainties in continuum
subtraction. For a few objects we could not locate any existing
published data of suitable accuracy, and these images lack calibrated
zero points. Uncalibrated data are indicated in the tables and figures.
For images which contain multiple sources with published photometry in
the same frame (e.g., the Perseus Cluster field), an average calibration
was computed and applied to all galaxies in that image including those
without existing photometry. Such galaxies have been flagged in
Table 4 and have larger photometric
uncertainties, since this method does not allow for individual color
term corrections. We note that the lack of an absolute calibration does
not affect the comparison between the shapes of the surface
brightness profiles
(Figs. 4b -
22b), or in certain derived photometric
parameters such as half-light radii.
4.4. Image Atlas
This UV/optical atlas consists of images and associated radial light and
color profiles. In Figures 4a -
22a we present the registered, multiband
images of the primary targets;
Figures 23a -
23b show thumbprints of UIT images for
the secondary targets. Objects are presented in order of increasing
right ascension. Where available, an
H and R-band image
are displayed for comparison to the FUV ("UIT 15") and MUV ("UIT 25")
images. In cases where
H is not available, or the
galaxy does not appear as a source in the FUV image, a B-band
and/or V-band image has been substituted. Images are oriented
north-up, east-left, and all images for a specific galaxy are displayed
with the same spatial scale. The adopted color tables and displayed
intensity ranges have been optimized for each individual galaxy in order
to emphasize extended, low surface brightness UV
structure. Morphological types were obtained from the
NASA/IPAC
Extragalactic Database (NED) and the Third Reference Catalog of Bright
Galaxies
(de Vaucouleurs et
al. 1991,
hereafter RC3).
4.5. Photometry
In Figures 4b -
22b we present azimuthally averaged
radial surface brightness and color profiles for the primary
objects. The FUV, MUV,
H, and R-band
profiles are shown, where available. For objects lacking
H data, B-band
photometry has been substituted. Arrows on the data points, oriented in
either an up or down direction, represent lower and upper limits,
respectively. The
H surface photometry is
presented in magnitudes, defined by -2.5 log10(f),
where f is in units of ergs s-1
cm-2. Surface brightness profiles which are uncalibrated are
flagged in the legend with "NC." Photometric errors, representing 1
standard deviation, are indicated on the profiles, generally for the
outermost points. For the larger galaxies in this sample, scaling of the
profiles in Figures 4b -
22b precludes display of the detailed
structure of the inner light profiles, but these data are available in
Table 9 (see
Appendix B). In most cases, the FWHM of the
seeing disk for the optical data was smaller than the FWHM of the UIT
data; this mismatch can produce spurious color gradients for r
5" in some sources.
For each primary object synthetic aperture photometry was performed
using the calibrated, unregistered, artifact-corrected images. The
photometry employed concentric fixed elliptical annuli centered on the
peak emission determined from the R-band image (where available,
or alternatively B band). The location of the central peak was
typically in agreement with the position given in the
RC3.
The width of the annuli ranged from 28" (25
UIT pixels) for the outermost regions of the galaxies having the largest
angular size, to a minimum of 3".3 (3 UIT pixels) for the innermost
annuli. In order to include any possible extended low surface brightness
structure around the objects, the outermost apertures were chosen to lie
well beyond the D25 isophotal diameter given in the
RC3.
The derived light profiles were individually
examined to determine the radius for which the surface brightness
profile flattened to the background sky.
Aperture parameters were determined by fitting ellipses to the outer
R-band (or B-band) isophotes for each object. The derived
ellipticity and position angles for a given object were used to
photometer all of the available bandpasses. For most objects, the
adopted position angle and ellipticity closely agreed with values given
in the
RC3.
Values for these parameters are presented in
Table 5.
Table 5. Photometric Parameters
|
OBJECT
(1) | l(deg)
(2) | b(deg)
(3) | FOREGROUND
EXTINCTION | D25/2(arcsec)
(7) | PA(deg)
(8) | b/a
(9) | SKY (mag
arcsec-2)
|
AB
(4) | A15
(5) | A25
(6) | µ15
(10) | µ25
(11)
|
|
| Primary Objects
|
|
| NGC 221...
| 121.2
| -22.0
| 0.33
| 0.67
| 0.58
| 261
| 170
| 0.7
| 22.0
| 24.1
|
| NGC 224...
| 121.2
| -21.6
| 0.33
| 0.67
| 0.58
| 5704
| 35
| 0.3
| 22.3a
| 25.4a
|
| NGC 598...
| 133.6
| -31.3
| 0.19
| 0.38
| 0.33
| 2119
| 23
| 0.6
| 22.3
| 24.7
|
| NGC 628...
| 138.6
| -45.7
| 0.13
| 0.26
| 0.23
| 313
| 25
| 0.9
| 23.9
| 24.5
|
| NGC 1068...
| 172.1
| -51.9
| 0.05
| 0.10
| 0.09
| 212
| 70
| 0.9
| 22.4
| 25.3
|
| NGC 1275...
| 150.6
| -13.3
| 0.75
| 1.51
| 1.31
| 65
| 110
| 0.8
| 23.3
| 25.4
|
| NGC 1316...
| 240.2
| -56.7
| 0.0
| 0.0
| 0.0
| 360
| 50
| 0.7
| 23.4
| 25.1
|
| NGC 1317...
| 240.0
| -56.7
| 0.0
| 0.0
| 0.0
| 82
| 78
| 0.9
| 23.5
| 25.3
|
| NGC 1399...
| 236.7
| -53.6
| 0.0
| 0.0
| 0.0
| 207
| ...
| 1.0
| 23.4
| 25.2
|
| NGC 1404...
| 237.0
| -53.6
| 0.0
| 0.0
| 0.0
| 99
| ...
| 1.0
| 23.5
| 25.5
|
| NGC 2146...
| 135.7
| 24.9
| 0.33
| 0.67
| 0.58
| 180
| 135
| 0.6
| 24.0
| 25.8
|
| NGC 2992...
| 249.7
| 28.8
| 0.27
| 0.54
| 0.47
| 106
| 15
| 0.3
| 22.3
| 26.0
|
| NGC 2993...
| 249.8
| 28.8
| 0.27
| 0.54
| 0.47
| 40
| 95
| 0.7
| 22.1
| 25.4
|
| NGC 3031...
| 142.1
| 40.9
| 0.16
| 0.32
| 0.28
| 806
| 157
| 0.5
| 24.4
| 25.8
|
| NGC 3034...
| 141.4
| 40.6
| 0.13
| 0.26
| 0.23
| 336
| 65
| 0.4
| 24.2
| 24.7
|
| UGC 5336...
| 142.0
| 41.1
| 0.16
| 0.32
| 0.28
| 75
| ...
| 1.0
| 26.3
| 25.3
|
| UGC 6697...
| 234.1
| 73.0
| 0.0
| 0.0
| 0.0
| 56
| 137
| 0.2
| 22.5
| 0b
|
| NGC 4151...
| 155.1
| 75.1
| 0.0
| 0.0
| 0.0
| 189
| 50
| 0.7
| 21.9
| 27.6
|
| NGC 4321...
| 271.1
| 76.9
| 0.06
| 0.12
| 0.10
| 222
| 30
| 0.9
| 20.0
| 21.6
|
|
| Secondary Objects
|
|
| Mrk 335...
| 108.8
| -41.4
| 0.11
| 0.22
| 0.19
| 9
| ...
| 1.0
| 21.6
| 25.0
|
| NGC 891...
| 140.4
| -17.4
| 0.32
| 0.65
| 0.56
| 404
| 22
| 0.2
| 23.2
| 25.2
|
| NGC 1267...
| 150.4
| -13.4
| 0.75
| 1.51
| 1.31
| 33
| ...
| 1.0
| 22.7
| 24.8
|
| NGC 1268...
| 150.4
| -13.4
| 0.75
| 1.51
| 1.31
| 29
| 56
| 0.7
| 23.1
| 24.9
|
| NGC 1270...
| 150.5
| -13.4
| 0.75
| 1.51
| 1.31
| 44
| 15
| 0.8
| 23.0
| 25.1
|
| NGC 1272...
| 150.5
| -13.3
| 0.75
| 1.51
| 1.31
| 61
| ...
| 1.0
| 23.0
| 25.0
|
| NGC 1273...
| 150.5
| -13.3
| 0.75
| 1.51
| 1.31
| 33
| ...
| 1.0
| 22.9
| 25.3
|
| UGC 2665...
| 150.5
| -13.2
| 0.75
| 1.51
| 1.31
| 31
| 122
| 0.4
| 22.8
| 25.5
|
| NGC 1277...
| 150.6
| -13.2
| 0.75
| 1.51
| 1.31
| 29
| ...
| 1.0
| 22.9
| 25.1
|
| NGC 1278...
| 150.6
| -13.2
| 0.75
| 1.51
| 1.31
| 46
| ...
| 1.0
| 22.9
| 25.2
|
| NGC 1282...
| 150.7
| -13.3
| 0.75
| 1.51
| 1.31
| 42
| 25
| 0.8
| 23.2
| 25.4
|
| NGC 1396...
| 236.7
| -53.7
| 0.0
| 0.0
| 0.0
| 30
| ...
| 1.0
| 23.4
| 25.3
|
| NGC 2551...
| 141.0
| 32.5
| 0.07
| 0.14
| 0.12
| 50
| 55
| 0.7
| 23.4
| 28.3
|
| NGC 3837...
| 234.4
| 72.9
| 0.0
| 0.0
| 0.0
| 19
| ...
| 1.0
| 22.6
| 26.5
|
| MCG 3-30-71...
| 234.8
| 72.9
| 0.0
| 0.0
| 0.0
| 26
| ...
| 1.0
| 23.2
| 26.5
|
| NGC 3842...
| 234.3
| 73.0
| 0.0
| 0.0
| 0.0
| 42
| 5
| 0.7
| 23.1
| 25.2
|
| CGCG 97-114...
| 235.1
| 73.0
| 0.0
| 0.0
| 0.0
| 3
| ...
| 1.0
| 22.6
| 24.6
|
| NGC 4156...
| 154.8
| 75.0
| 0.0
| 0.0
| 0.0
| 42
| ...
| 1.0
|
error bars in this and
all proceeding surface brightness and color profiles (for inner radii,
the error bars are smaller than the symbol sizes). (b)
UV/optical extinction-corrected radial surface brightness
(upper) and color (lower) profiles for NGC 221. Note that
offsets (given in the legend) have been applied. The R-band data
are from
Kent (1987).
