scientific abstract exploration of the nature, physical conditions and evolution of the nuclear regions of luminous external galaxies is the main purpose of the sws cp proposal: galactic nuclei. we propose to carry out multi-line spectroscopy for a detailed study of the circum-nuclear interstellar media and for a better determination of the properties of the central energy source(s). we will first explore the global character of the circum-nuclear gas by observing the brightest infrared lines in a sample of about 60 galaxies of all classes, including normal, starburst and distant luminous iras galaxies, as well as seyferts, liners and agn/qsos. in a next step we will then study physical properties and excitation of the circumnuclear regions of a selected group of galaxies in more detail by observing a wide range of ionic, atomic and molecular infrared lines. due to the large gain in sensitivity and the full wavelength coverage, such a program will only become possible with the advent of iso. with the help of theoretical modeling and comparison to nearby, prototypical template. sources, these measurements will determine the physical processes in and constrain current evolutionary models of galactic nuclei. observation summary we plan to take advantage of the spectroscopic capabilities of iso over its full wavelength range, using the following aots: sws: medium resolution spectroscopy with the aots sws01,sws02,sws06 lws: medium resolution spectroscopy with aots lws01,lws02 pht: low resolution spectra with aot pht40 for a small number of template. sources, we will perform scans over the full iso wavelength range. for all our program galaxies, we will obtain a survey of some of the brightest or most important lines: species lambda mg v 5.608 ar iii 8.991 ne v 14.320 (only in ir-luminous galaxies+n5253+n6764+iizw40+izw1+mk463) s iii 18.713 o iv 25.913 s iii 33.480 si ii 34.814 o iii 51.815 (or lws full scan) o i 63.184 .. c ii 157.741 .. pht-s spectrum a subset of starburst galaxies will be studied in detail in a large number of lines characterizing various phases of the ism: species lambda br alpha 4.052 mgv 5.608 h2 s(5) 6.910 pf alpha 7.460 nevi 7.642 ariii 8.991 siv 10.511 h2 s(2) 12.279 neii 12.814 nev 14.320 neiii 15.555 h2 s(1) 17.035 siii 18.713 ariii 21.842 feiii 22.930 fei 24.042 nev 24.300 si 25.249 oiv 25.913 feii 25.988 h2 s(0) 28.219 siii 33.480 siii 34.814 feii 35.349 neiii 36.020 h2o 40.337 o iii 51.815 (from lws full scan) n iii 57.317 .. o i 63.184 .. o iii 88.356 .. n ii 121.898 .. o i 145.526 .. c ii 157.741 .. a search for molecular hydrogen emission (s(0) and s(2)) in galactic disks will be done for a number of mostly edge-on galaxies. the oh 34.6 line will be observed in the megamaser galaxies arp 220, mrk 231 and ngc3690a/bc, in coordination with lws. h3+ emission from x-ray illuminated gas will be searched for in ngc 6240 and ngc 1068. a subset of active galactic nuclei will be observed in the following lines tracing the nlr, clr, partially ionized and molecular zones: species lambda siix 2.585 mg viii3.028 siix 3.935 mgiv 4.488 mgvii 5.500 mgv 5.608 sivii 6.515 s(5) 6.910 nevi 7.642 mgvii 9.030 siv 10.511 s(2) 12.279 neii 12.814 mgv 13.540 nev 14.320 neiii 15.555 s(1) 17.035 siii 18.713 feiii 22.930 fei 24.042 nev 24.300 oiv 25.913 feii 25.988 s(0) 28.219 feii 35.349 neiii 36.020 for the two liners studied in detail, high excitation lines will be skipped we deviate from the philosophy to use both sws and lws by dropping lws observations for those sources in which the lws consortium will obtain equivalent data. concatenation is asked for only in a limited number of cases where the same aot is used at several positions, e.g. of an interacting system. a number of very long observations with aot sws02 have been split. these are deliberately not concatenated to allow efficient scheduling. for details see the scientific justification below. in particular, the quick overview of observations. indicates, for both positions of the hole, which sources are observed, to which level of detail, and the corresponding priority. the scientific justification contains also a list of requested s/n values for the various projects. in bright sources, these are often exceeded by large factors within the shortest possible integration times for the respective aots. for some faint lines in faint sources, the requested s/n cannot be met within the time limit of 1280s pure integration per line we have adopted for most sources. details on integration time per line for each source by far exceed the size limits imposed for this file. they are available on request. version march 7, 1994
Instrument
LWS01 , PHT40 , SWS01 , SWS02 , SWS06
Temporal Coverage
1996-02-04T14:27:30Z/1998-01-15T20:02:24Z
Version
1.0
Mission Description
The Infrared Space Observatory (ISO) was the worlds first true orbiting infrared observatory. Equipped with four highly-sophisticated and versatile scientific instruments, it was launched by Ariane in November 1995 and provided astronomers world-wide with a facility of unprecedented sensitivity and capabilities for a detailed exploration of the Universe at infrared wavelengths.
European Space Agency, Genzel et al., 1999, 'Infrared Spectroscopy of Bright Galactic Nuclei and the Connection between Star Formation and AGNs. Part 1 of 3 ', 1.0, European Space Agency, https://doi.org/10.5270/esa-zw33a3g
