Nancy A. Oliversen, Joy Nichols-Bohlin, and Matthew P. Garhart. Astronomy Programs, Computer .... 5 11 09.3 -67 51 32. 5 11 49.8 -7005 25. 5 2449.2 -7007 37.
NASA Reference Publication 1203 June 1988
International Ultraviolet Explorer Spectral Atlas of Planetary Nebulae, Central Stars, and Related Objects
Walter A. Feibelman Nancy A. Oliversen Joy Nichols-Bohlin Matthew P. Garhart
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NASA Reference Publication 1203
International Ultraviolet Explorer Spectral Atlas of Planetary Nebulae, Central Stars, and Related Objects
Walter A. Feibelman Goddard Space Flight Center Greenbelt, Maryland Nancy A. Oliversen Joy Nichols-Bohlin Matthew P. Garhart Computer Sciences Corporation Beltsville, Maryland
Series Organizer: Jaylee M. Mead Goddard Space Flight Center
National Aeronautics and Space Administration Scientific and Technical Information Division
IUE SPECTRAL ATLAS OF PLANETARY NEBULAE, CENTRAL STARS, AND RELATED OBJECTS Walter A. Feibelman Laboratory for Astronomy and Solar Physics, NASA-GSFC and Nancy A. Oliversen, Joy Nichols-Bohlin, and Matthew P. Garhart Astronomy Programs, Computer Sciences Corporation
INTRODUCTION Nine years of observations with the International Ultraviolet Explorer (IUE) satellite have resulted in a data bank of approximately 180 objects in the category of planetary nebulae, their central stars, and related objects. Most of these objects have been observed in the low dispersion mode with both the short wavelength (SWP) and long wavelength (LWR or LWP) cameras. Although numerous papers have appeared in the recent literature based on these observations, the published data represent various aspects selected for specific purposes and are often processed by widely varying methods. Thus, until now, there has not been available a comprehensive atlas of ultraviolet spectrograms of these objects. The overwhelming majority of the spectra in this reference atlas were taken through the large (10" X 20") entrance aperture, thus resulting in spectra that contain information on the nebular spectrum, as well as that of the central star. The low-dispersion IUE spectra also provide spatial information along the long axis of the large aperture, which is perpendicular to the direction of dispersion, and can therefore be used for a line-by-line analysis. Approximately 40 objects are of large angular diameter relative to the IUE entrance apertures and low nebular intensity so that the central stars were observed without nebular contamination. For about 15 nebulae of sufficient brightness and angular extent, the large or small aperture was purposely offset from the central star so as to obtain a nebular spectrum uncontaminated by the central star. One of the surprising results of these studies has been the realization that no two planetary nebulae have identical spectra in the ultraviolet region, even if their optical spectra are very similar. THE ATLAS The ultraviolet observations of planetary nebulae obtained with the IUE during the past 9 years represent an enormous investment in observing time and a most valuable repository of spectral information for these objects. To make this information generally available to the astronomical community, we have prepared this reference atlas, which contains the best representative samples of ultraviolet low-dispersion observations of planetary nebulae that are currently available. The reference atlas consists of 177 plots, which are shown in a standardized format and arranged by Right Ascension. Table 1 gives the following information: Col.(l) The plot number. Co1.(2) The object name, usually by its NGC, IC, Abell, or other most common designation.
Co1.(3) Right Ascension (RA) and Declination (DEC) (1950 epoch), taken from the IUE Merged Log of Observations for the illustrated spectra. The coordinates in the merged log are provided by the guest observer on the observing "script." Slight variations for the coordinates may be found in the Merged Log of Observations of duplicate observations due to individual guest observers using coordinates from different sources, or purposely having chosen the "center of light'' of the object in question. If the target is relatively bright (i.e., greater than about 10th magnitude) and is centrally condensed, then the IUE can center on the target even if the coordinates supplied by the guest observer are in error by an arcminute or two. Objects with differing coordinates for the LWR and SWP spectra are noted in Table 1 by an asterisk; at the end of the table, we give additional comments of our best estimates on how well the positions of the SWP and LWR spectra agree. Co1.(4) and (5) The SWP image sequence number and exposure time. C01.(6) and (7) The LWR (or LWP) image sequence number and exposure time. C01.(8) The wavelength point at which the SWP and LWR (LWP) spectra were spliced together. Co1.(9) Name of the Principal ~nvestigatorprogram for the respective spectra shown. Col.(lO) Additional comments concerning the quality of the spectra, such as s a t u ~ t i o n off, sets, or identification of objects that are not planetaries, i.e., symbiotics, HI1 regions, etc. As much as possible we have tried to present flux calibrated spectra using, where necessary, various correction algorithms for known calibration errors. To begin with, the net flux (Flux Number, or FN) was obtained from the merged extracted low-dispersion file (MELO) supplied by the IUE Spectral Image Processing System (IUESIPS). The exposure time used was generally that supplied by the comments given in the science header. The absolute calibration of Bohlin and Holm (1980) was then applied to the SWP and LWR spectra, while the calibration of Cassatella and Harris (1982) was applied to the LWP spectra. The IUE image processing system has evolved during the past 9 years of IUE operation. The "new" low-dispersion processing system was implemented on November 4, 1980, at the Goddard Space Flight Center (GSFC) and on March 10, 1981, at the Villafranca del Castillo (VILSPA) observatory. The main improvement of the "new" calibration was to double the spectral extraction frequency and to increase the apparent resolution of the spectra. However, therc is no significant flux calibration difference between the two processing methods in the low-dispersion mode. Thus, whenever possible, the most recent optimally exposed spectra were selected.
Table 1 Spectra of Planetary Nebulae, Central Stars and Related Objects Contained in the Atlas Plot No. (1) 1 2 3 4 5
Object
1950 Coordinatesa RA DEC 0 I I H M S (3) 0 10 18.0 +72 14 00 0 16 01.0 +53 35 41 0 30 33.1 -71 58 32 03444.9 -135927 0 39 26.0 -73 01 43 I
(2) NGC 40 Vy-1 SMC N2 BB-1 SMC N5
SWP Image Exposure No. min (4) (5) 3074 8
-
-
20527 20591 20453
90 120 80
LWR Image No. (6) 2656 3090
Exposure min (7) 8 90
-
-
16515
113
-
-
14706
2
-
-
15738 10043 13850
180 175 80
6 7 8 9 10
NGC 246 SMC N43 SMC L302 SMC N87 M1-1
04432.8 04924.5 05435.0 11957.0 1 34 12.9
-120843 -74 1 3 5 4 -722300 -733000 +50 12 57
18642 20455 16210 13387 17571
45s 33 180 180 70
11 12 13 14 15
NGC 450 M1-2 K1-26 P136+5.1 CPD-26 389
13911.0 1 55 32.9 2 55 09.8 25931.9 3 31 03.2
+51 1 9 0 0 +52 39 15 -44 22 20 +ti44257 +26 02 18
11239 19289 21421
986 1 15323
55 90
-
-
21015 66 18
60 120 15 270
-
-
37s
5680
2m 20s
16 16 17 18 19
IC351 IC351 NGC 1514 NGC 1535 M4-18
3 3 4 4 4
+34 +34 +30 - 12 +60
17574 21158 18042 10737 9659
28 120
8206
45
-
-
40 3m 20s 180
14219 2232 8401
15 5 90
20 21 22 23 24
LMC P2 A-7 5-320 LMC N97 LMC P9
4 48 27.0 50051.8 5 02 48.2 5 05 04.0 5 0 8 17.3
44 44 06 11 21
20.2 20.2 08.0 54.0 17.9
53 53 39 52 00
35* 35 00 00* 00
-72 33 27 -154033 +10 38 25 -68 43 00 -684402*
Merge Point A (8) 1950 1890 1950 1950 1950
(9) Perinotto Johnson Maran CleggIBarlow Maran
1950 1950 1950 1920 1950
Kaler Maran BarlowIWillis Barlow Aller
1950 1950 1950
Pottasch Feibelman Kaler
CIV, CIII], and NIII? or noise spike at 2960 CS
1950 1920
Heckathorn Sion
CPD-26 389 is CS of NGC 1360
1950 1950 1950 1950 1950
AllerIBoggess Aller Seaton HeapIBoggess Peimbert Maran GreenISeaton Boggess Barlow Maran
20422 10279 7967 14199
45
-
-
2x30 32 120
14212 6939
65 35
-
-
1950 1940 1950 1950
20424
72
16472
120
1950
PI^
CommentsC
SWP/LWR(P) (10) SWP reprocessed
CIV, CIII] sat
CS
CIII] sat
several ext pixels HeII, CIV, CIII] sat CS CS; many ext pixels
CS; SWP: 2 expo in LGAP BSP? 1832 A BSP? 1400 A
A sat
Table 1 continued Spectra of Planetary Nebulae, Centml Stars and Related Objects Contained in the Atlas Plot No.
Object
H (2) LMC N28 LMC NllO LMC N133 IC 418 LMC N201
5 5 5 5 5
1950 Coordinatesa RA DEC M S o (3) 11 09.3 -67 51 32 1 1 49.8 - 7 0 0 5 25 2449.2 - 7 0 0 7 37 25 09.5 -12 44 15 25 39.0 -71 35 00 t
t I
Image No. (4) 13409 19486 19481 665 1 14216
SWP Exposure min (5) 190 160 168 2 150
LWR Image No. (6) 12474
Exposure min (7) 80
-
-
2257
I
-
-
Merge Point A (8) 1950 1950 1950 1950 1950
PI^ SWP/LWR(P) (9) Barlow Barlow Barlow Lutz/Boggess Barlow
CommentsC (10) BSP 1509 A
LMC N141 LMC N203 LMC P33 LMC N66 NGC 2022
Barlow WillisIBarlow Maran Barlow Czyzak
FD 73 IC 2149 IC 2149 K 1-27 LMC P40
WillisIBarlow Hamngton Ham ngton Kaler Maran
PW- I IC 2165 5-90 A-15 NGC 2346
KalerIWeinberger Czyzak BoggessICzyzak Perinotto Pottasch
CS
NGC 2346 A-20 NGC 2371 NGC 2392 Y M-29
Feibelman Kaler Pottasch Aller Kaler
Variable CS
LGAP centered on CS; SWP: some ext data LGAP offset 5.4"E + 4.1"N of CS CS CIV, CIII] sat
CS; ext data 1300 Variable
A
Fix; LGAP offset 6.1"W CS; LWR: few ext pixels
+ 2.1"s
of CS
Table 1 continued Spectra of Planetary Nebulae, Central Stars and Related Objects Contained in the Atlas Plot No. (1) 50 51
Object (2) VV 1-7 NGC 2440 NGC 2440 NGC 2440 NGC 2440
1950 Coordinatesa RA DEC o I ! I H M S (3) 7 38 59.9 -18 51 59 73941.5 -180526
SWP Image Exposure No. min (4) (5) 8866 3 ~ ( 3 m10s) 17243 6
LWR Image Exposure No. min (6) (7)
-
-
13507
12
Merge Point A (8) 1950 1950 1950 1950 1950
PI" SWP/LWR(P) (9) Heap Ferland Ferland Ferland Ferland
CommentsC (10) SWP: 3 exposures in LGAP Centered on CS Centered on CS; CIV, HeII, CIII], NeIV sat LGAP offset 9.O"W + 4.3"N from CS LGAP offset 9.O"E + 4.3"s from CS
+
NGC 2452 NGC 2610 A-28 M3-6 A-3 1
1950 1950 1950 1950 1940
AllerlPottasch Kaler Kaler Seaton Kaler
SWP: 19.12m NB Ping 2600 A
IC 2448 NGC 2792 NGC 2867 A-33 IC 2501
1950 1950 1940 1950 1940
GrewingJSeaton Pottasch Aller HeapJKaler Seaton
Sat data 2800 A BSP near CIV Fix
1950 1950 1950 1890 1940
Kaler Prevot Bohlin SeatonIBarlow Grewing
CS; ext data 1200-1350 A LGAP centered on CS; ext data 2650-2900 LGAP offset 15"E from CS CIV, HeII, CIII], [NeIV], 0111 sat
1950 1950 1960 1950 1950
Boggess Ferland Aller Aller Barker
LGAP offset 6.6"W 2.4"N of CS; CIII] sat LGAP centered on CS LGAP offset 7.2"E + 2"N of CS; LWR ping 2890-3020 LGAP offset 3.3"W 7.3"s of CS; several lines sat 12"N of CS SMAP offset 9"W
A-34 NGC 3 132 NGC 3132 IC 2553 NGC 3195 NGC NGC NGC NGC NGC
321 1 3242 3242 3242 3242
-
-
LWP 2796 5325 15880 13754
13 120 65 33
180m CS
Ext data 2600-2870 A CS
A
+
+
+
A
Table 1 continued Spectra of Planetary Nebulae, Central Stars and Related Objects Contained in the Atlas
(2) AG Car NGC 3587 K1-22 NGC 4361 IC 3568
1950 Coordinatesa RA DEC H M S (3) 105410.0 -6011 10 11 11 55.0 +55 17 00 1 1 24 17.5 - 3 4 0 5 4 4 12 21 54.8 -18 30 28 1231 46.6 +I325022
80 81 82 83 84
LT-5 H4-1 LO-8 A-36 VV-68
12 12 13 13 13
85 86 87 88 89
He2-108 IC 4406 Hen 1044 NGC 5882 Me2-I
14 14 48.0 14 19 15.5 145614.7 15 1325.0 15 19 23.0
90 91 92 93 94
He2-131 CN 1-1 SP-1 He2-138 NGC 6026
95 96 97 98 99
NGC 6058 Sand 3 IC 4593 A-39 NGC 62 10
Plot No. (1 75 76 77 78 79
Object
O
Image No. (4)
3542 16327 16969 19903 13875
SWP Exposure min (5) 80s 60 70 4 15
LWR Image Exposure No. min (6) (7) 31 15 40s 12579 60 IS879 10509
9 20
Merge Point A (8) 1950 1950 1950 1940 1950
-
CommentsC
PI" SWP/LWR(P) (9) Johnson Seaton Kaler Barlow Harrington
(10) SWP reprocessed; Nebulae around WN9 star Mainly CS; ext data 1200-1350 CS
A
NV ext, ext data 2800
A
17236 20599 8237 14215 8000
10 60 4 lm 20s 30
13502 16513 7186 678 1 6963
10 60 6 2m 30s 30
1950 1890 1940 1950 1940
Kaler Barlow Barlow KalerISeaton Grewing
MgII sat CIII] sat CS CS also NGC 5135
-51 57 00 -43 55 27 -540609 -452800 -23 27 05
17067 23420 5567 16349 5233
45 60 60 30 9
10776 LWP 3725 4805 12599 45 17
27 60 40+10 31 30
1940 1950 1940 1940 1940
SeatonIBarlow Grewing Purton Seaton Aller
Probably not a PN; Fix; LWR: 2 exposures in LGAP;
153154.0 15 47 3 8 5 15 47 56.7 1551 19.0 155807.0
-714500 -48 36 00 -51 22 23 -660000 -342400
6772 13665 17732
6 30 60
9547 10293
4 75
-
6720 16348
4 35
5735 12597
3 30
SeatonIHeck Lutz Kaler Seaton
CS
-
1940 1940 1950 1940 1950
Seaton
SWP: Image header lists incorrect expo. time
160243.4 16 03 12.0 160923.3 16 25 32.2 16 42 24.0
+404904 -35 37 00 +I21208 +28 01 12 +23 54 00
10 14293 27 6721 2m30s 6646 40 17237 10733 3x (5m 20s)
10913 5765 5705 15846 9422
20 20 4 82 3x 6m
1950 1950 1950 1950 1940
Kaler Seaton Lutz Kaler Heap
CS
53 57 22 37 50
07.8 02.8 45.0 57.4 10.0
+26 +27 -37 -19 -66
09 44 54 20 21 00 37 47* 16 00
Fix; CD-22 12238 is the CS of Me2-1
CS; high extinction CS
CS CS 3 exposures in LGAP; NV ext
Table 1 continued Spectra of Planetary Nebulae, Central Stars and Related Objects Contained in the Atlas Plot No. (1) 100 101 102 103 104
(2) IC 4634 M2-9 CPD-56 8032 IC 4642 A-41
1950 Coordinatesa RA DEC I I! H M S (3) 16 58 34.0 -21 45 12 170252.5 -100431 17 04 48.0 -56 51 00 17 07 36.0 -55 20 00* 1 7 2 6 10.3 -15 1 0 4 5
105 106 107 108 109
K1-14 He2-274 MI-26 NGC 6445 HI-36
17 40 29.3 17 41 53.0 174245.1 17 46 17.0 17 46 24.1
+21 -46 -30 -19 -37
110 11 1 1 12 113 1 14
A43 NGC NGC NGC NGC
6543 6565 6563 6572
1 7 5 1 11.0 17 58 34.0 18 0842.2 180845.0 180941.9
+I03800 +66 38 05 -28 11 22 -335300 +064959
10245 1897 24266 17029 8669
1 15 116 117 118 119
NGC 6567 SWST 1 K1-16 A46 NGC 6644
18 10 48.0 18 12 58.0 18 21 35.3 182918.0 18 29 30.0
-19 05 00 -30 53 00 +64 20 30 +265405 -25 10 00
120 121 122 123 124
IC 4776 Hu 2-1 NGC 6720 NGC 6720 NGC 6720
18 42 34.0 18 47 39.1 18 51 43.4 18 51 46.0 185143.4
-33 24 00 +20 47 11 +32 57 49 +32 58 07 +325808
Object
28 04 10 59 00
17 00 53 41* 34*
SWP Exposure rnin (5) 35 150 55 80 300
Image No. (4) 20578 20662 8947 10507 22456 27899 13413 20579 17030 5566
70 4 157 180 60
LWR Image Exposure No. min (6) (7) 16497 15 25 16571 7700 25 5734 40 16938 200 -
-
10078 16498 4507 5802
7m 30s 200 90 30
85 4 60 120 15
8735 1761 LWP 461 1
60 4 60
-
-
742 1
17019 10035 17235 9473 1734
186 20 20 45 30
16504 8589 7230 7231 7219
30 40 60 90 60
Merge Point A (8) 1950 1950 1950 1950 1950
plb SWP/LWR(P) (9) Clegg Feibelman Heck PerinottoISeaton Bond
CommentsC (10)
HeII?, CIIIOIIIlMgI? sat CS
1950 1950 1950 1940 1940
Kaler Barlow Clegg PottaschIAller PurtonIAllen
CS Also TC- I ; ext data 2600-2900 Also HD 3 16248
ClavelISeaton Daltabuit Aller Pottasch Czyzak
CS SWP reprocessed; 1250-1450
12
1950 1950 1950 1950 1940
13307 10077 13501 8203 1630
60 7 35 40 40
1950 1940 1950 1940 1940
Pottasch SeatonIBarlow Kaler Boggess Boggess
CIV CIII] sat; extlsat 1200-1350
12764 5703 6238 6239 6222
30 40 90 90 30
1950 1940 1950 1950 1940
Pottasch Boggess/Lutz Barker Barker Barker
A
SS; Fix
A, CIV sat
CIII] sat
A
CS: much of LWR sat Fix; CIII] sat [OII] ext CS in LGAP but offset 7.4"E + 2.1"s from CS; LGAP offset 16"N 42.8"E of CS LGAP offset 7.8"E + 16"N of CS
+
Table I continued Spectra of Planetary Nebulae, Central Stars and Related Objects Contained in the Atlas Plot No. (1 125 126 127 128 129
Object H (2)
1950 Coordinatesa RA DEC I 1 M S (3) 58 06.0 - 18 17 00 00 02.0 -00 31 12 12 30.8 +28 35 26 1354.0 - 3 9 4 1 0 0 15 49.3 -01 41 24 0
Image No. (4) 16935 5213 17729 13920 6643
SWP Exposure min (5) 120 70 80 58 80
LWR Image Exposure No. min (6) (7)
Merge Point
PI^ SWP/LWR(P) (9) Perinotto Aller Kaler AllerIBoggess Lutz
CommentsC (10)
A-5 1 NGC 6741 K3-27 IC 1297 NGC 6778
18 19 19 19 19
NGC 6790 NGC 6803 BD +30°3639 HM Sge NGC 6818
19 20 25.0 192853.5 19 32 47.9 193941.1 19 41 09.4
+01 25 00 +095700 +30 23 59 +I63733 -14 16 21
15411 6256 8590 13548 13944
90 60 5 10 15
Seaton Harrington Boggess Boggess Aller
CIII] sat
NGC 6826 NGC 6826 NGC 6826 A-65 V1016 Cyg
19 43 27.0 194327.0 19 43 27.0 19 43 34.3 19 55 20.0
+50 24 00 +502400 +50 24 00 -23 15 36 +39 41 24
16328 14626 14616 18641 22891
Im 30s 60 20 165 2
-
-
LWP 3261
2
Seaton Helfer Helfer Kaler Feibelman
LGAP centered on CS LGAP offset 8.6"W 4.8"s of CS; CIII] sat LGAP offset 4.8"E + 8.6"s of CS CS SS
V1016 Cyg NGC 6853 NGC 6853 NGC 6853 NGC 6884
19 19 19 19 20
+3941 +22 35 +22 34 +22 33 +46 18
25 17 100 240 180
LWP 4959 5515 13676 14790 1784
25 30 120 180 40
Nussbaumer Bohlin Barker Barker PottaschIDaltabuit
SS; many lines sat LGAP centered on CS
FG Sge NGC 6886 NGC 6891 IC 4997 NGC 6905
20 09 43.0 201029.6 20 12 48.0 20 1751.0 2 0 2 0 9.0
55 57 57 57 08
19.9 30.0 26.4 20.7 49.1
39 24656 00 6406 32 17420 18737 49 44* 17018
+20 1 1 00
-
-
+I95016 +12 33 00 +I63427 +I95600
8983 8864 14400 13405
240 3x8 30 20
Cassatella Aller HeapISeaton Feibelman Barlow
CS Fix CIV, HeII, CIII] sat; LWR image no. wrong in label
SS; MgII, 0111, [ArIV], 0111 sat LGAP offset 4.9"E + 4.3"N of CS; [NeIV] sat
+
LGAP offset 48"W + 27"s of CS LGAP offset 127"W + 70"s of CS
CIII], 0111 sat SWP: 3 exposures in LGAP CIII], [OII], MgII sat
Table 1 continued Spectra of Planetary Nebulae, Central Stars and Related Objects Contained in the Atlas Plot No. (1) 150
Object H (2)
1950 Coordinatesa RA DEC M S (3) 28 54.0 -07 16 00 47 40.0 +13 22 00 49 02.6 +35 23 37 49 02.6 +35 23 37 59 05.0 +54 21 00 0
I
11
Merge Point A (8) 1950 1950 1940 1950 1950
SWP/LWR(P) (9) Perinotto Perinotto Feibelman Nussbaumer PottaschISeaton
PI^
CommentsC (10)
A
-
35
LWP 6919
30
9387 9053 1739 19877 17242
7 10 40 12 180
743 1 7804 1633 15862 15861
8 25 20 27 180
1940 1940 1950 1950 1950
LutzICzyzak Boggess Boggess Barlow FerlandIBarlow
LGAP centered on CS LGAP offset 8"W of CS Fix
+ I 1 5700 +392440 +31 28 18 12 33 49 -39 37 28
17069 13339 19907 14289 16968
60 47 4 12 60
13360 885 1 15881 10774
60 80 6 18
-
Seaton MatsonIAller Kaler Kaler/Barlow Kaler
in M 15; CIII] sat
-
1890 1950 1940 1950 1950
+50 +2 1 +59 +42 +42
45 32 45 34 37
7257 19832 19770 6467 6466
72 5 35 6 12
5429 15828 15782 5548 5547
36 14 25 12 9
1940 1950 1950 1950 1950
Hanington Drilling Kaler Bohlin Bohlin
+42 15 41 +575400 +483232 +48 32 32 +48 32 32
20095 17075 9080 27202 27202
30 150 20 15 15
16036 13359 7827 LWP 7217 LWP 7217
60 120 21 15 15
1950 1940 1950 1950 1950
Barker Seaton Plavec Oliversen Oliversen
20 20 20 20 20
NGC NGC NGC NGC NGC
210129.9 210127.6 21 04 35.0 21 05 09.4 21 05 09.4
-113359 -113354 +47 39 03 +42 02 01 +42 02 03
K648 HU 1-2 A-78 NGC 7094 IC 5148
21 21 21 21 21
2734.0 31 6.9 33 20.1 34 27.9 56 33.0
IC 5217 NGC 7293 Wein- 12 NGC 7662 NGC 7662
22 22 23 23 23
21 26 10 23 23
NGC 7662 HB- 12 Z And Z And Z And
23 23 29.4 232357.0 2 3 3 1 15.3 23 31 15.0 23 31 15.0
56.0 55.0 02.7 28.7 30.0
LWR Image Exposure No. min (6) (7) -
A-70 A-72 HBV 475 HBV 475 NGC 7008 7009 7009 7026 7027 7027
SWP Exposure Image min No. (4) (5) 13765 150
+
42 05 19 15 15
CS; Bsp 1340 CS Variable SS Variable SS; MgII ext CS; LWR: 20h 59m 6.8s
Many lines sat
CS CS
CS Small HI1 region; extlsat data 2640-2970 A 1.5"s of CS LGAP offset 6.8"W LGAP offset 6.9"E + 1"N of CS; CIV, Hell, CIII] sat
+
SMAP offset 4"N of CS SS, quiescent state; several lines sat SS, in outburst; LGAP; several lines sat SS, in outburst; SMAP
Table 1 continued Spectra of Planetary Nebulae, Central Stars and Related Objects Contained in the Atlas Plot Object No. (1) (2) 175 Jn- 1 176 A-82
1950 Coordinatesa RA DEC H M S (3) 23 33 24.1 +30 11 26 23 43 20.6 +56 47 21 0
I
I'
SWP Image Exposure No. min (4) (5) 15104 85 19908 120
LWR Image Exposure No. min (6) (7) -
-
-
-
Merge Point A (8) 1950 1950
pIb SWP/LWR(P) (9) Ualer Kaler
CommentsC (10) CS CS
Comments: RA and DEC were obtained from the IUE merged log. An asterisk in the DEC column indicates that the coordinates listed in the IUE merged log were different for the SWP and LWR spectra. For these cases the SWP coordinates are given in the RA and DEC columns above while the LWR coordinates are given in the comments below. Please refer to the additional comments given below about the centering of the individual spectra. Note that the coordinates listed in the IUE merged log are supplied by the guest observer and may be subject to small errors (see discussion in text). If the Principal Investigator for the SWP and LWR(P) spectra.were the same only one PI was listed. sat = saturated data, ext = extrapolated data, Bsp = bright spot, Fix = SWP spectrum corrected for SWP ITF error CS = central star, SS =-symbiotic star, NB = nebulae LGAP = large aperture (10" ~ 2 0 " ) . SMAP = small aperture (3" diameter circle)- The LGAP was used unless otherwise specified.
"
Additional notes concerning the positioning of the SWP and LWR spectral pairs:
16 IC 351 18 NGC 1535 24 LMC P9 42 5 - 9 0 60 IC 2448 63 A-33 83 A-36 103 IC 4642 108 NGC 6445
144 NGC 6884
LWR 1950 coordinates: RA DEC +34' 54' 00" 3h 44m 18s - 12' 51' 42" 4h 1 lm 57s 5h 8m 16.7s -68' 43' 59" 6h 23m 00s 17' 49' 00" 9h 06m 37s -69' 44' 07" 9h 36m 37.1s - 2' 34' 57" 13h 37m 58s -19' 37' 33" 17h 07m 37s -55' 20' 00" 17h 46m 17.0s - 19' 59' 41"
+
Probably same position. FES centering was used. Position uncertain. The quality of the SWP and LWR merge is only "fair." FES centering was used. Position uncertain. The SWP coordinates may not be correct because the spacecraft was moved prior to the start of the SWP exposure. Probably same position. FES centering was used. Probably same position. The SWP and LWR merge together well and FES centering was used. Position uncertain. Blind offsetting techniques were used. The quality of the merge of the SWP and LWR spectra appear to be ok. Probably same position. The SWP and LWR merge together well. Probably same position. The SWP and LWR merge together well. Position uncertain. The coordinates for the SWP and LWR are the same however some drift may have occurred during the LWR exposure. Position uncertain. FES centering was used, however FES counts for the target are not consistent between the SWP and LWR observations. Position uncertain. The SWP and LWR merge together well. FES centering was used, however the FES counts for the target are not consistent between the SWP and LWR observations. Probably same position. FES centering was used.
For a small number of objects, where only a single, early observation was available, reprocessing to avoid calibration errors has been necessary. Early SWP images suffer from an error in the 2 0 percent intensity transfer function (ITF) level (Holm, et. al., 1982). Approximately 6 percent of the atlas objects were affected by the ITF error. This ITF error was corrected by the use of a procedure (SWPFIX), which is available at the Goddard Regional Data Analysis Facility (RDAF). Each LWR spectrum has also been corrected for the sensitivity degradation of the LWR camera using the wavelength dependent correction algorithm of Clavel, Gilmozzi and Prieto (1986). Comparable wavelength dependent correction algorithms for the SWP and LWP cameras do not yet exist. The resolution of the IUE Project's routine sensitivity monitoring analysis is too coarse for use for this atlas. Consequently, no sensitivity degradation correction has been applied to either the SWP or LWP spectra. The degradation in the SWP and LWP cameras is 2-4 times less than for the LWR camera (Sonneborn and Garhart 1986). Other than the corrections mentioned above, we present the data "as taken," i.e., without smoothing or filtering out noise spikes (like the one at 2200 A), since such procedures may also lose information. Some of the plots contain regions with low signal-to-noise levels that can drop below the zero flux level. Such low signal-to-noise levels are typically due to regions on the IUE cameras with lower sensitivity (e.g., near 2200 for the LWR), or just plain underexposure. Such objects may be candidates for reobservation if of sufficient importance. Furthermore, due to the uncertainty of extinction values we decided to present the observed data without corrections for interstellar absorptions. For large values of the logarithmic extinction at HP, C, the slope of the continuum at the short-wavelength end is greatly steepened when corrected for the appropriate extinction, and the corresponding absolute flux values may change by a large amount. A good example of this is the central star spectrum of Sp-1 (see Kaler and Feibelman 1985). Each calibrated spectrum is shown in its entirety, if available, from 1200 A to 3200 A on a 30-cm by 10-cm Calcomp plot, with tic marks every 100 A second plot shows the same object on an expanded vertical scale to bring out the weaker features but truncates the stronger emission lines. For each plot, an SWP and an LWR (or LWP) spectrum were spliced together at a position where the two plots appeared to blend relatively smoothly together. In most cases, the splice point was chosen to be at 1950 in order to avoid splitting the C 1111 1909 emission line. For a few objects the splice point was chosen to be at 1890 when the C 1111 line was saturated in the SWP spectra but not in the LWR spectra. Occasionally it was unavoidable to include spectra which contained saturated data and/or data extrapolated above the highest level of the ITF. The reseau marks have been indicated on the spectra by crosses along the lower wavelength axis, while the saturated and/or extrapolated data have been indicated by crosses along the upper wavelength axis. In Table 2, adapted from Koppen and Aller (1987), we show a list of the most common emission lines found in planetary nebulae in the IUE spectral range. The last plot in the atlas locates the more prominent of these wavelength identifications from which the user may want to make a transparent overlay.
A
A.
A
A
A
SUPPLEMENTAL INFORMATION For a complete listing of all objects in category 70 (planetary nebulae plus central stars) and 71 (planetary nebulae minus central star), as well as the symbiotics, HI1 regions and related objects, the reader is referred to the IUE Merged Log of Observations which is updated periodically. A browse file of the photowrite images obtained with IUE from Goddard is available for
Table 2 Lines Observed in Planetarv Nebulae (Adapted from Koppen and Aller 1987)
Wavel.
1 175176 1239143 1309 1335136 1371 1 39411403 1397- 1407 1483187 1548150 1575 1602 1 640 1658-66 1718 171 1 1747-54 1760 1815 1808117 1882192 1907109 2253 2297 2306 2321131 2325-29 2334-50 2385
Identification
Lo
Hi
Excitation
17 10 9 9 29 9 9 9 8 8 8 49 8 23 14 7 16 7 7 7 7 54 18 54
coll? coll, wind coll coll, diel. rec. wind, rad. coll coll coll coll coll coll rec coll wind, diel. rec. coll? coll rec coll coll coll coll rec diel. rec. rec
CIII NV SiII CII OV
2~ 3 ~ - 2 p 2 3~ 2s 2s-2p 2PO 3p 2@-3p2 2~ 2p 2p0-2p 2~ 2p I@-2p2 I D
6 0 0 0 20
SiIV OIV] NIV] CIV [NeVl [NeIV] He11 01111 NIV SiII NIII] CII [ NeIII] SiII SiIII] CIII] HeII CIII He11 [0111] CII]
3s 2 ~ - 3 p 2Po 2p 2p0-2p2 4~ 2s2 IS-2p 3P0 2s 2s-2p 2PO
0 0 0 0
[SiII] He11
2p2 3~-2p2 IS 2p3 4~0-2p3 2~ Balmer alpha 2p2 3~-2p3 5P 2p IF-2p2 I D
0 0 41 0 16
3p2 2 ~ - 5 f 2p 2p 2p0-2p2 4~ 2p2 2 ~ - 3 p 2P 2p4 3~-2p4 I S 3p 2P-3p2 2~ 3s2 IS-3p 3@' 2s2 Is-2p 3 P Paschen 6
7 0 9 0 0 0 0 48
2p 'Po-2p2 I D Paschen epsilon 2p2 3 ~ - 2 IS~ ~ 2p *Po-2p2 4~
13 48 0 0
3p 2p0-3p2 4~ Paschen delta
0 48
6 6
coll coll
6 54
coll rec
Table 2 continued
inspection at GSFC and a file of images obtained from VILSPA is currently being processed at GSFC. A master tape of spectra in this atlas has been generated and is available at the Regional Data Analysis Facilities to guest observers and other interested colleagues. A bibliographical index of all published data on planetary nebulae based on IUE data up to the end of 1985 is contained in IUE NEWSLETTER No. 30. This compendium by Mead, Brotzman, and Kondo (1986) lists the names of almost 9600 objects observed by IUE and identifies 1 133 refereed papers, arranged alphabetically by names of first authors, that have appeared in main journals. Copies of thc Newsletters are available from the IUE project. We plan to update the atlas after the IUE satellite's termination. In the meantime, the semiannual editions of Astronomy and Astrophysics Abstracts serve as a useful list of updated references.
Lines Observed in Planetary Nebulae (Adapted from Koppen and Aller 1987)
Wavel. 2423125 2470 251 1 2663 2696 2723 2733 2763 278412929 2786 279612803 279112797 2829 2837138 2837 2852 2854168 2929137 2929 2945 2973179 3023 3043147 306317 1 3 10913005 3133 3188 3203
Identification [NeIV]
Lo
Hi 6 6 54 24 24 24 54 24 4 4 4 9 24 16 41 4 4 9 4 24 43 37 37 4 4 41 24 54
[or11 He11 He1 He1 He1 He11 He1 [MgVl
2p3 4~-2p3 2~ 2p3 4~-2p3 2~ Paschen gamma 2s 3 ~ l-p ~3 ~ 0 2s 3 ~ - 9 p 3 ~ 0 2s S-8p 3 ~ 0 Paschen beta 2s 3 ~ - 7 p 3 ~ 0 2p4 3~--2p4 I D
[ArVl MgII MgI1 He1 CII 0111
3p2 3~-3p2 IS 3s 2 ~ - 3 p 2 ~ o 3p 2@-3d 2~ 2s 3 ~ - 6 p 3 ~ 0 2p2 2 ~ - 3 p 2 ~ o 3p 3 ~ - 3 d 3@
0 0 48 20 20 20 48 20 0 0 0 4 20 12 36
MgI [ArIV] MgII
3s2 IS-3p IP0 3p2 4~-3p2 2~ 3p 2@-4s 3 2p4 3 ~ - 2 p 4 I D 2s 3 ~ - 5 p 3 ~ 0 3p 2 ~ - 3 d 2@ 3s 3p0-3p 3~ 3s 3Po-3p 3~ zP2 3 ~ - 2 p 2 IS 3p4 3~-3p4 IS 3p 3~-3d 3p0 2s 3 ~ - 4 p 3p0 Paschen alpha
0 0 4 0 20 38 33 33 0 0 37 20 48
[MgVl He1 NIII 0111 0111 IN111 [ArIII] 0111 He1 He11
Excitation coll coll rec rec rec rec rec rec coll coll coll coll? rec rec Bowen fluo. coll coll coll? coll rec ? ?? Bowen fluo. Bowen fluo. coll coll Bowen fluo.
We thank Keith Feggans for retrieving much of the original data from the National Space Science Data Center files for us. Support for this atlas provided by NASA IUE contract NAS5-28749 with CSC for the Archival Program NAGWF is gratefully acknowledged.
REFERENCES Bohlin, R. C. and Holm, A. 1980, NASA IUE Newsletter, 10, 37. Cassatella, A. and Harris, A. 1982, IUE ESA Newsletter, 17, 12. Clavel, J. Gilmozzi, R., and Prieto, A. 1986, NASA IUE Newsletter, 31, 83. Holm, A., Bohlin, R. C., Cassatella, A., Ponz, D. P. and Schiffer, F. H. 1982, Asrron. Astrophys., 112, 341. Kaler, J. B. and Feibelman, W. A. 1985, Astroph. J., 297, 724. Kbppen, J. and Aller, L. H. 1987, Exploring the Universe With the IUE, p. 589, ed. Y. Kondo, Reidel: Dordrecht. Mead, J. M., Brotzman, L. E., and Kondo, Y., 1986, NASA IUE Newsletter, 30. Sonnebom, G. and Garhart, M. P. 1986, NASA IUE Newsletter, 31, 29.
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