2006A&A...452..523K


C.D.S. - SIMBAD4 rel 1.7 - 2021.02.24CET22:12:38

2006A&A...452..523K - Astronomy and Astrophysics, volume 452, 523-535 (2006/6-3)

Multi-aperture photometry of extended IR sources with ISOPHOT. I. The nature of extended IR emission of planetary nebulae.

KLAAS U., WALKER H.J., MUELLER T.G., RICHARDS P.J. and SCHREIBER J.

Abstract (from CDS):

ISOPHOT multi-aperture photometry is an efficient method to resolve compact sources or to detect extended emission down to relatively faint levels with single detectors in the wavelength range 3 to 100µm. Using ISOPHOT multi-aperture photometry and complementary ISO spectra and IR spectral energy distributions we discuss the nature of the extended IR emission of the two PNe NGC6543 and NGC7008. In the on-line appendix we describe the data reduction, calibration and interpretation methods based on a simultaneous determination of the IR source and background contributions from the on-source multi-aperture sequences. Normalized profiles enable direct comparison with point source and flat-sky references. Modelling the intensity distribution offers a quantitative method to assess source extent and angular scales of the main structures and is helpful in reconstructing the total source flux, if the source extends beyond a radius of 1arcmin. The photometric calibration is described and typical accuracies are derived. General uncertainty, quality and reliability issues are addressed, too. Transient fitting to non-stabilised signal time series, by means of combinations of exponential functions with different time constants, improves the actual average signals and reduces their uncertainty. The emission of NGC6543 in the 3.6µm band coincides with the core region of the optical nebula and is homogeneously distributed. It is comprised of 65% continuum and 35% atomic hydrogen line emission. In the 12µm band a resolved but compact double source is surrounded by a fainter ring structure with all emission confined to the optical core region. Strong line emission of [ArIII] at 8.99µm and in particular [SIV] at 10.51µm shapes this spatial profile. The unresolved 60µm emission originates from dust. It is described by a modified (emissivity index β=1.5) blackbody with a temperature of 85K, suggesting that warm dust with a mass of 6.4x10–4M is mixed with the ionised gas. The gas-to-dust mass ratio is about 220. The 25µm emission of NGC7008 is characterised by a FWHM of about 50'' with an additional spot-like or ring-like enhancement at the bright rim of the optical nebula. The 60µm emission exhibits a similar shape, but is about twice as extended. Analysis of the spectral energy distribution suggests that the 25µm emission is associated with 120K warm dust, while the 60µm emission is dominated by a second dust component with 55K. The dust mass associated with this latter component amounts to 1.2x10–3M, significantly higher than previously derived. The gas-to-dust mass ratio is 59 which, compared to the average value of 160 for the Milky Way, hints at dust enrichment by this object.

Abstract Copyright:

Journal keyword(s): techniques: photometric - astronomical data bases: miscellaneous - infrared: ISM - planetary nebulae: individual: NGC6543 - planetary nebulae: individual: NGC7008 - methods: data analysis

CDS comments: Table A.6 objects with format N NNNN not identified.

Simbad objects: 72

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Number of rows : 72

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 HD 344 HB* 00 08 03.4867829686 -33 31 45.573921330   6.787 5.662     K1III 31 0
2 * bet Cas dS* 00 09 10.68518 +59 08 59.2120 2.73 2.61 2.27 1.97 1.77 F2III 502 0
3 IRC +10011 OH* 01 06 25.9889735162 +12 35 52.890666456   20.7   18.26 14.01 M8 405 0
4 * bet And PM* 01 09 43.92388 +35 37 14.0075 5.58 3.62 2.05 0.81 -0.19 M0+IIIa 538 0
5 OH 127.8 -0.0 OH* 01 33 51.21 +62 26 53.2           M9III 175 0
6 * 49 Cet PM* 01 34 37.7788265080 -15 40 34.898112472   5.667 5.607   5.54 A1V 254 0
7 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1115 1
8 * alf Ari PM* 02 07 10.40570 +23 27 44.7032 4.29 3.17 2.01 1.15 0.54 K2-IIIbCa-1 609 1
9 * omi Cet Mi* 02 19 20.79210 -02 58 39.4956   7.63 6.53 5.03   M5-9IIIe+DA 1456 0
10 * tau01 Eri PM* 02 45 06.2034405658 -18 34 21.478629972 4.94 4.94 4.46 4.03 3.76 F7V 214 0
11 V* ET Eri AB* 03 31 03.9163734978 -15 24 52.011622030   13.97 12.25 11.20   M6 24 0
12 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1733 1
13 IC 2006 EmG 03 54 28.427 -35 58 01.75   12.39   10.94 11.9 ~ 196 0
14 * alf Tau LP? 04 35 55.23907 +16 30 33.4885 4.32 2.40 0.86 -0.37 -1.31 K5+III 1192 1
15 HD 34700 TT* 05 19 41.4088548858 +05 38 42.777125431 9.75 9.788 9.15 8.80 8.47 G0IVe 74 0
16 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1694 1
17 IRAS 09371+1212 pA* 09 39 53.96 +11 58 52.6           K7II/III 159 0
18 HD 97048 Ae* 11 08 03.3105687971 -77 39 17.491180130 9.03 8.76 9.00   8.64 A0Vep 467 0
19 HD 97300 Ae* 11 09 50.0178181814 -76 36 47.711452436   9.41 9.20   8.82 B9V 162 1
20 HD 98800 RS* 11 22 05.28975 -24 46 39.7571   10.20 9.28 9.26 7.386 K5V(e) 335 0
21 * bet Leo dS* 11 49 03.57834 +14 34 19.4090 2.30 2.22 2.13 2.08 2.06 A3Va 548 0
22 V* T Cha Or* 11 57 13.5268556629 -79 21 31.521755129   10.00 11.86     K0e 241 1
23 V* UW Cen RC* 12 43 17.1899844640 -54 31 40.763053503   10.84 10.13     K 108 0
24 V* Y CVn C* 12 45 07.8257032577 +45 26 24.898861195 14.03 7.41 4.87 3.12 1.74 C-N5 463 0
25 V* V854 Cen RC* 14 34 49.4088471574 -39 33 19.276531885   7.13 11.69     Ce 201 0
26 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 374 1
27 HD 135344 * 15 15 48.9457954324 -37 08 55.727525343   7.84 7.76     A0V 130 1
28 V* RS Lib Mi* 15 24 19.7909563744 -22 54 39.822052678   10.59 7.00     M7-8e 119 0
29 V* WX Ser Mi* 15 27 47.0424743675 +19 33 51.669514287           M8.5 199 0
30 HD 139614 Ae? 15 40 46.3818973118 -42 29 53.538928508   8.47 8.24     A9VekA5mA5(_lB) 167 0
31 * g Lup PM* 15 41 11.3769921 -44 39 40.342813   5.036 4.633     F3/5V 184 0
32 V* R CrB RC* 15 48 34.4147978750 +28 09 24.298218765 6.44 6.31 5.71 5.26 5.08 G0Iep 762 0
33 HD 142666 TT* 15 56 40.0222941557 -22 01 40.004849949 9.41 9.37 8.82 8.31 8.01 F0V_sh 225 0
34 HD 144432 Ae* 16 06 57.9530266912 -27 43 09.758016578 8.47 8.53 8.19 7.82 7.53 A9/F0V 218 1
35 V* V856 Sco Ae* 16 08 34.2868591379 -39 06 18.326059778 7.66 7.41 7.05 6.92   A7IIIne_sh 359 0
36 V* V1027 Sco a2* 16 08 34.5611688784 -39 05 34.277434873   6.552 6.629 6.66   A0/3III 179 0
37 NGC 6090 PaG 16 11 40.3 +52 27 21   14.0       ~ 402 2
38 IRAS 16342-3814 pA* 16 37 39.8700524769 -38 20 17.440442399           ~ 128 0
39 * c Oph Be* 17 31 24.9541340 -23 57 45.513592 4.75 4.81 4.81 4.74 4.72 A0V 257 0
40 HD 161796 pA* 17 44 55.4696057799 +50 02 39.477383602 8.00 7.68 7.21 6.77 6.51 F3Ib 313 0
41 V* T Dra C* 17 56 23.3278798922 +58 13 06.827212507   18.08 7.20     C6,2e 175 0
42 * gam Dra * 17 56 36.36988 +51 29 20.0242 5.630 3.760 2.230 1.08 0.23 K5III 521 0
43 NGC 6543 PN 17 58 33.4042519454 +66 37 58.748961810   11.09 11.28     [WC] 1128 1
44 V* VX Sgr s*r 18 08 04.0431479808 -22 13 26.629744195 11.72 9.41 6.52 3.90 2.11 M8.5Ia 556 0
45 HD 169142 Ae* 18 24 29.7799676975 -29 46 49.328597698   8.42 8.16     F1VekA3mA3_lB? 352 2
46 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2537 0
47 * ome Pav PM* 18 58 36.4483714404 -60 12 01.991511383 7.95 6.51 5.14     K2IIICNIV 57 0
48 HD 176386 Y*O 19 01 38.9314887024 -36 53 26.560961605 7.28 7.44 7.32 8.11   B9V 120 0
49 V* TY CrA Ae* 19 01 40.8312189956 -36 52 33.801844387 10.03 9.92 9.39     B9e 272 0
50 V* V Aql C* 19 04 24.1548619887 -05 41 05.434251344   11.09 6.90     C-N5 206 0
51 HD 179218 Ae* 19 11 11.2540715594 +15 47 15.632212730 7.55 7.476 7.39 7.25 7.21 A0Ve 225 0
52 V* W Aql S* 19 15 23.3581458294 -07 02 50.308513461   12.72 10.14     S6/6e 209 0
53 V* RY Sgr RC* 19 16 32.7669543079 -33 31 20.337025534 6.20 6.27 6.25     Cpec 356 0
54 * chi Cyg S* 19 50 33.9243904 +32 54 50.609683 7.02 6.06 4.24 1.81 -0.01 S6-9/1-2e 670 0
55 V* NS Vul LP? 19 52 30.0760 +22 27 14.376 8.96 8.68 7.76 5.07 2.33 A2 59 0
56 V* QT Tel LP* 19 55 54.6743051872 -51 23 30.077858628           ~ 5 0
57 IRAS 19575-4317 * 20 01 00.4906669400 -43 09 30.775987927           ~ 2 0
58 IRAS 20174-7853 * 20 24 35.5324229536 -78 44 09.591875530   13.480 11.707     ~ 3 0
59 IRAS 20240-2142 * 20 26 59.8703643285 -21 32 15.003452190   13.13 11.63     ~ 2 0
60 IRAS 20270-2858 * 20 30 03.3618204792 -28 48 49.695178089           ~ 4 0
61 * ome Cap V* 20 51 49.2909479855 -26 55 08.891176687 7.66 5.75 4.12 2.87 1.93 M0IIIBa0.5 96 0
62 NGC 7008 PN 21 00 32.817600 +54 32 35.37600       13.21   ~ 232 2
63 * mu. Cep s*r 21 43 30.4610574 +58 46 48.160181 8.85 6.43 4.08 1.98 0.22 M2-Ia 629 1
64 NSV 25875 OH* 22 19 27.48 +59 51 21.7           ~ 134 0
65 IRAS 22296+2004 Mi* 22 32 01.1785205905 +20 19 55.042156228           ~ 5 0
66 V* HM Aqr pA* 22 35 27.5256072315 -17 15 26.885199823 9.31 9.08 8.90     A0III 102 0
67 IC 1459 GiP 22 57 10.60677155 -36 27 43.9953697   10.96 11.85 9.34 10.3 ~ 583 2
68 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1135 3
69 * iot Gru SB* 23 10 21.5375522 -45 14 48.164650   4.877 3.877     K1III 72 0
70 * gam Tuc PM* 23 17 25.7507806263 -58 14 08.707239934 4.35 4.37 3.98 3.57 3.33 F4V 151 0
71 RAFGL 3068 C* 23 19 12.60744 +17 11 33.1332           C 256 0
72 V* R Cas Mi* 23 58 24.8700291935 +51 23 19.691977266 6.71 6.63 4.80     M6.5-9e 685 0

    Equat.    Gal    SGal    Ecl

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2021.02.24-22:12:38

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