<=== observer ===>
"RGENZEL",\
"Genzel, R.",\
"",\
"Max-Planck-Institut fuer extraterrestrische Physik",\
"Giessenbachstrasse",\
"1603",\
"85740",\
"Garching b. Muenchen",\
"Germany",\
"49 89 32993614",\
"49 89 32993569",\
"lutz@mpe-garching.mpg.de",\
<=== proposal ===>
"MPEXGAL1", 1, 4,\
{"active galactic nuclei",\
"compact galaxies",\
"normal galaxies",\
"quasars",\
"starburst galaxies"},\
{"D. Lutz",\
"A. Eckart",\
"H. Feuchtgruber",\
"A. Moorwood",\
"T. de Graauw",\
"E. Valentijn",\
"J. Koornneef",\
"M. Kessler",\
"A. Sternberg",\
"H. Netzer",\
"D. Hollenbach"}
<=== title ===>
Infrared Spectroscopy of Bright Galactic Nuclei and the Connection
between Star Formation and AGNs. Part 1 of 3
<=== abstract ===>
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 VIII]3.028
[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
<=== scientific_justification ===>
Time distribution (for both launch windows)
Team Total 1st 2nd 3rd priority
SWS 435600 174240 130680 130680
AFM 115200 43200 36000 36000
SOT 32400 12960 9720 9720
-------------------------------------
583200 230400 176400 176400
Our observing program can be separated into 4 sub-sections which differ in
scientific goal, number of sources and number of lines. These sub-projects are
described in turn in the following paragraphs. Whereas the proposal is
structured into these subprojects for clarity, actual observations of
individual sources will collect in one go all requirements that may
originate from the subprojects, in order to avoid overheads.
We aim at detecting most lines at a signal to noise ratio of 10 or better.
For the adopted line-to-continuum ratios, this transforms into the minimum
continuum S/N ratios listed below. Exceptions where this goal is not achieved
are a few faint lines or faint sources where we have limited the
integration time per source and per line to no more than 1280 secs.
Upper limits e.g. for high excitation lines in ultraluminous IRAS galaxies
may nevertheless be important constraints for the possible contribution
of AGNs to the energy output of these objects. Similarly, we have limited
the time for an LWS01 observation to not more than 0.5 hours including the
separate background spectrum.
Complete Spectral Scans of Template Sources:
In this part of our program we plan to perform complete spectral scans (2.4 -
200 microns) on the prototypical `template' sources described above. The
scientific goal here is to obtain unbiased, complete SWS and LWS spectra
of sources that can be considered 'pure' or well studied cases and that can
be used to refine the physical modelling described above.
These spectra also serve to find unexpected, serendipitous spectral features.
They will detect lines expected to be bright but not included in our line
lists for detailed spectroscopy in order to keep them focussed to a subset best
serving our diagnostic aims. This is e.g. the case for several fine-structure
lines from star forming regions, planetary nebulae, and the NLR and CLR
of active galaxies.
The measurements will be carried out with the AOT SWS01, using the mode for
full SWS resolution, and the Medium Resolution Spectrum (LWS01) AOT of LWS.
Bright Line Survey:
In this project we wish to explore the global characteristics of 8 of the
brightest far-infrared emission lines in all program galaxies
(plus the templates for calibration purposes). We have selected for study the
19 um and 34 um [S III] (SWS) and the 52 um [O III] lines (LWS) as probes of
moderate density, photoionized gas, for which a first density estimate may
be derived from the ratio of the [S III] lines. The 158 um [C II], 63 um
[O I] (LWS) and 34 um [Si II] (SWS) lines have been selected as probes of
moderate and high density neutral atomic gas in photodissociation regions
and shocks. Measurements of [O IV] 26 um will probe for the presence of
high excitation gas. For the ultraluminous IRAS galaxies, the discrimination
between starburst and AGN energy sources will be strengthened by an additional
search for the [NeV] 14.32um line (EP 97 eV). Due to the ability to
simultaneously observe in the two sections of SWS, we will be able to
supplement this list at no cost by a survey of another line from photoionized
gas, [Ar III] 9.0 um, and a survey for the coronal line [Mg V] 5.6 um, which
however will in most cases yield only upper limits. ISOPHOT-S spectra will
relate these observations to the properties of dust features, and allow to
deduce Lyman contiuum fluxes from Br alpha for some of the brighter sources.
Because of the low spectral resolution and resulting low line-to-continuum
ratio, only the very brightest lines can be seen in the PHT-S spectra.
Summary of observations for the bright line survey:
Species Lambda Minimum S/N on continuum
[Mg V] 5.608 -
[Ar III] 8.991 5
[Ne V] 14.320 50 (only in IR-luminous galaxies+N5253+N6764+IIZW40+IZw1+Mk463)
[S III] 18.713 10
[O IV] 25.913 50
[S III] 33.480 20
[Si II] 34.814 20
[O III] 51.815 (LWS full scan, S/N>20 for the most difficult lambda~52um)
[O I] 63.184 ''
[C II] 157.741 ''
PHT-S Spectrum
Note: LWS01 fullscan replaced by LWS02 line spectra of 63.184 and 157.741 for
sources with S(60um) < 5Jy.
>From this data set we expect to be able to derive a first order impression on
the global physical conditions and excitation (temperature, density) of the
ionized and atomic interstellar media of galaxies of all types and get a census
on the range of line luminosities in each type of galaxy.
Due to the faintness of F10214+4724 (S_25um = 0.075 Jy) and its high
redshift, it is not feasible to obtain comprehensive infrared spectroscopy
as for the other sources in our sample. We will study 6 lines in the SWS
range, ranging from relatively low excitation ([Ne II], [ArII]) to higher
excitation ([ArIII],[OIV],[S IV]) and very high excitation ([NeVI],[SiIX]),
in an attempt to classify the exciting radiation field as starburst-like or
AGN like. [Ne II] emission with a line-to-continuum ratio as observed for
the M82 starburst would be detected with high significance in the proposed
integration time, whereas [S IV] emission scaled to the observed H alpha
according to our Seyfert model could be detected in the case of AGN
excitation.
The SWS-AOT used for the Bright Line Survey is SWS02 with R~1000. For active
galaxies known to exhibit very broad `narrow' lines (e.g. 19254-7245), we
will instead use SWS06 to cover a broader range around the line center. LWS
observations are done using the Grating Wavelength Range Spectrum (LWS01)
AOT for sources brighter than 5 Jy at 60um. Even for a moderate number of
lines, this maximises the scientific output with respect to the instrumental
overheads. For the fainter sources, will will only observe the lines [O I]
63.2um and [C II] 157.7um, using AOT LWS02 to scan 5 resolution elements
centered on each line.
PHT-S spectra (AOT P40) for sources brighter than 4 Jy at 12um will be
obtained with an integration time corresponding to a S/N ratio of at least
100-200 at 12um. For fainter sources, integration time will be limited to
512s (on-source), still allowing studies of dust features at reduced S/N.
In most cases, we do not plan to take separate background spectra close to
our sources, in order to avoid the additional time overhead of a factor of 2.
The infrared background far from the galactic plane is typically ~0.2 Jy
within a SWS beam and ~2 Jy within a LWS beam. For the SWS observations,
the background signal is comparable to the source signal only for the fainter
sources. The continuum fluxes of these sources are well known from IRAS
observations, and possible line contamination by galactic emission can
be separated kinematically. For LWS, background spectra will be taken
for all except the template sources. PHT-S observations use a chopping AOT.
Detailed Spectroscopy of Star-Forming Galaxies:
In this section of our program we hope to determine the character of the
radiation field (intensity and effective temperature of the UV field),
constrain the range of excitation conditions in the ionized gas and explore
the properties of the molecular interstellar medium in detail in a set of
normal, star-forming and luminous IRAS galaxies, IR-bright AGN galaxies
and the templates. The goal is that for these galaxies ~30 different ionic,
atomic and molecular lines are then available that cover a wide range of
excitation conditions. We expect that these galaxies will form the basic
data set for a detailed comparison of observation and theoretical modeling
of the different physical processes discussed throughout our proposal.
For this purpose we have selected a larger number of atomic and molecular
lines, and require measurements of higher accuracy for some of the survey
lines.
We will test the hypothesis that all galaxies that are characterized as
star bursters on the basis of their far-infrared continuum properties can in
fact be explained by photoionization of molecular clouds by a OB-star radiation
field.
Various lines of [S III], [S IV], [Ne II], [Ne III], [N II], [N III], [O III],
[O IV], [Ar III] will sample ionized gas in ionization stages from 14 to 55 eV
that can be reasonably expected from gas ionized by normal OB stars. The
ratios of the [O III], [Ne III], [S III] and [Ar III] lines will give accurate
electron densities.
We have selected the 14 and 24 um [Ne V] and 7.6 um [Ne VI] lines to determine
the excitation and density of a possible hot coronal medium generated by
supernova explosions and investigate existence and physical conditions of
hidden AGNs.
In total, the lines of four different ionization states of neon
will sample the ionizing radiation field over a wide range of energies
without interference from abundance or depletion effects.
We will also observe 4 um HI 5-4 and 7 um HI 6-5 for determining emission
measures (Lyman continuum fluxes) and extinctions in the same beam as used
for the fine structure lines. The combination of fine structure lines and
recombination lines will also give a measure of abundances.
145 um [O I], 25 um [S I], transitions of [FeI], [FeII] and [FeIII], the
H_2 pure rotational transitions S(0), S(1), S(2), S(5) and 40 um H_2O
(6_43 - 5_32) are selected to probe dense, warm atomic and molecular material
in photodissociation regions and shocks. The mid-IR [FeII] lines, together with
well-known near-IR transitions, provide powerful constraints on the properties
of partially ionized gas. [Fe III] observations will help to determine the
Fe abundance / depletion.
The 4.35um and 16.33um transitions in H3+ have been proposed as a unique
spectral signature of X-ray excited gas (Draine and Woods 1990). This
may however change in the light of re-evaluations of H3+ recombination rates.
A limited attempt do detect these lines in N6240 and N1068 is made.
Summary of observations for detailed spectroscopy of starforming galaxies:
(including bright line survey lines)
Species Lambda Minimum S/N on continuum
Br alpha 4.052 10.
[MgV] 5.608 -
H2 S(5) 6.910 333.
Pf alpha 7.460 50.
[NeVI] 7.642 333.
[ArIII] 8.991 50.
[SIV] 10.511 50.
H2 S(2) 12.279 100.
[NeII] 12.814 50.
[NeV] 14.320 100.
[NeIII] 15.555 100.
H2 S(1) 17.035 100.
[SIII] 18.713 100.
[ArIII] 21.842 333.
[FeIII] 22.930 333.
[FeI] 24.042 333.
[NeV] 24.300 333.
[SI] 25.249 333.
[OIV] 25.913 333.
[FeII] 25.988 333.
H2 S(0) 28.219 333.
[SIII] 33.480 100.
[SiII] 34.814 100.
[FeII] 35.349 333.
[NeIII] 36.020 333.
H2O 40.337 100.
[O III] 51.815 (LWS full scan, S/N > 40 for the most difficult lambda~52um)
[N III] 57.317 ''
[O I] 63.184 ''
[O III] 88.356 ''
[N II] 121.898 ''
[O I] 145.526 ''
[C II] 157.741 ''
The observations will be performed with AOT SWS02 at a resolution of 1000
and with LWS01 full scans. Time estimates for this section of our program
have been derived using the line-to-continuum approach.
SWS02 spectra of H3+ 4.35 and 16.33 have been added only for NGC6240 and
NGC 1068.
The OH 34.6 line will be observed in the megamaser galaxies Arp 220, Mrk 231
and NGC3690A/BC, in coordination with LWS.
For NGC 4945, the 0-0 S(7) and 1-0 Q(3) lines of molecular hydrogen have
been added, and the required S/N for the molcular hydrogen lines has been
increased.
For a number of edge-on systems covering a range of far-infrared luminosities,
we will obtain off-nuclear SWS02 spectra in the lines of H_2 S(0) 28.219
and H_2 S(2) 12.279 offset by D25/2 from the nucleus. The SW section of SWS
will simultaneously be aimed at the H_2 S(7) 5.5112 and H_2 1-0 Q(3) 2.432
lines.
Detailed Spectroscopy of AGNs:
In this section of our program we have selected bright Seyfert 1s, Seyfert 2s,
NLXGs, Liners and two radio-selected AGNs. Detailed spectroscopy will be
obtained probing gas in the NLR and CLR ([Ne II], [Ne III], [Ne V], [Ne VI],
[S III], [S IV], [O IV], [Mg IV], [Mg V], [Mg VII], [Mg VIII], [SiVII],
[Si IX]). The aim is to get a full description of the parameters of the
infrared emission in the NLR/CLR, including densities from various line ratios
at different levels of excitation.
The H_2 S(0),S(1),S(2),S(5) lines, together with the [Si II] line (already
observed in the bright line survey) will test the evidence for a warm, dense
molecular/atomic zone near the nuclear emission region (Note that models for
X-ray-illuminated molecular gas predict high intensities of the higher
rotational transitions of H_2). Again, [Fe II] and [Fe III] will prove to be
particularly useful in conjunction with NIR data. Including the lines that
were already observed in these sources during the survey these AGNs will
then be observed in lines that trace the active nucleus as well as lines that
are expected to be bright for star formation.
This project will thus provide a basic data set for testing models of the
NLR/CLR of AGNs, and test whether these prototype AGNs are also currently
forming stars. For the AGNs that are also template sources, this data set
will be complemented by line detections expected from the full scans.
Time estimates for this section have been derived using the approach
to scale the expected line emission with the dereddened Hbeta flux,
adopting predictions from photoionization models and a certain margin for
bright lines. Lines included in the survey (L/C-based) and in this project
([S III], [O IV]) will be observed according to the method predicting the
fainter line flux. Again, a limit of not more than 1280s pure integration
time per line has been enforced.
Summary of observations for detailed spectroscopy of AGNs:
Species Lambda I/Ihbeta_limit (to be detected with 10 sigma)
Seyferts Liners
[SiIX] 2.585 0.02 -
[MgVIII] 3.028 0.10 -
[SiIX] 3.935 0.05 -
[MgIV] 4.488 0.10 -
[MgVII] 5.500 0.20 -
[MgV] 5.608 0.10 -
[SiVII] 6.515 0.05 -
S(5) 6.910 0.02 -
[NeVI] 7.642 0.02 -
[MgVII] 9.030 0.20 -
[SIV] 10.511 0.50 -
S(2) 12.279 0.02 -
[NeII] 12.814 0.02 0.31
[MgV] 13.54 0.02 -
[NeV] 14.320 0.19 -
[NeIII] 15.555 0.50 1.60
S(1) 17.035 0.02 0.02
[SIII] 18.713 0.35 0.60
[FeIII] 22.93 0.10 -
[FeI] 24.042 0.10 -
[NeV] 24.300 0.07 -
[OIV] 25.913 0.50 0.01
[FeII] 25.988 0.10 -
S(0) 28.219 0.02 -
[FeII] 35.349 0.10 -
[NeIII] 36.020 0.15 0.11
Note: Not all coronal lines will be observed in N1275, CenA
Quick overview of observations
==============================
Note: This list is a merger of the two lists for different `hole' positions.
If a source shows up in several projects, observations with the same AOT
are merged to avoid overheads. Priorities are given for autumn/spring launch,
i.e. 1/2 means priority 1 for autumn launch and 2 for spring launch
Source Full scan Survey Detailed(SB) Detailed(AGN) H2 off-nuc
SWS SWS LWS PHT SWS LWS SWS SWS
------------------------------------------------------------------------
Templates:
GC SgrA 1/1 2/ 3/ 2/ *
GC Ring NE 1/ 2/ 3/ 2/
GC Ring SW 1/ 2/ 3/ 2/
RCW103 1/ 3/
IC443 /1 /3
30 Dor 1/1 2/2 3/3 3/3 2/2 3/3
W 51 1/ 2/ 3/ 2/ *
DR 21 /1 /2 /3 /3 /3 /3
M82 1/1 1/1 3/3 1/1
NGC 253 2/2 2/2 3/3 2/2 2/2
NGC 1068 1/1 1/1 3/3 1/1* 1/1
Circinus 1/ 1/ 1/ 3/ 1/ 1/ 1/
NGC 4151 1/1 1/1 3/3 1/1
Normal Galaxies/Dwarfs
NGC 891 1/1 3/ 3/3 1/1*3/ 2/2
NGC 4567 3/3 3/3 3/3
NGC 4568 3/3 3/3 3/3
NGC 5194 M51 3/3 3/3
IIZw40 /3*
He2-10 /3 /3 /3
NGC 6052 3/
HII Galaxies / Starbursts
IC 342 /2 /3 /2
NGC 1808 /1 /1 /3 /1 /1
NGC 3256 /1 1/1 1/1 3/3 1/1 1/1
NGC 3690/IC 694 A 2/2 3/3 2/2*
NGC 3690/IC 694 BC 2/2 3/3 2/2*
NGC 4945 1/ 3/ 1/ *
NGC 5236 M83 3/ 3/ 3/
NGC 1614 /3 /3 /3
NGC 2903 /3 /3 /3
NGC 3079 /2 /2 /3 /2
NGC 4038 3/3 3/3
NGC 4039 3/3 3/3
NGC 4038/39 overl. 3/3 3/3
NGC 5253 3/ *3/ 3/
F15564+6359 3/ 3/ 3/
NGC 6764 3/3 3/3
NGC 6946 3/3 3/3 3/3
NGC 7552 3/3 3/3 3/3 /3 /3
IR luminous / Mergers
Mrk 231 1/1 3/3 1/1*
Arp 220 1/ 3/ 1/1*
NGC 6240 1/ 3/ 1/1*
20551-4250 1/1 2/1 3/3 2/1 2/1
05189-2524 /1 /3 /1
06035-7102 /1 /2 /3
06206-6315 /2 /2 /3
08572+3915 /1 /3
09320+6134 UGC5101 1/1 3/3
F10214+4724 1/1*
12112+0305 1/1 3/3
13428+5608 Mrk273 1/1 3/3 3/3
14348-1447 1/ 3/
15250+3609 3/ 3/
17208-0014 1/ 2/ 3/
19254-7245 1/1 2/2 3/3
20100-4156 3/3 3/3 3/3
22491-1808 1/1 3/3
23128-5919 1/1 2/1 3/3 /2 /1
Seyfert 1s
NGC 1365 2/1 2/2 3/3 2/1
NGC 7469 2/2 2/2 3/3 2/2
NGC 3783 3/3 3/3
13224-3809 3/ *3/ 3/
Seyfert 2s
Mrk 6 /1 /3 /3 /1
Mrk 1 3/3 3/3 3/3
Mrk 573 /3 /3
NGC 1672 /3 /3 /3
Mrk 3 /3 /3
Mrk 34 3/ 3/ 3/
NGC 5643 3/ 3/ 3/
PKS 2048-57 3/3 3/3 3/3
NLXGs
NGC 7582 2/1 1/1 1/1 3/3 1/1
NGC 5506 2/ 3/ 2/
NGC 2992 /2 /2 /3 /3 /2
Liners
M 81 2/2 3/3 2/2
NGC 4569 3/3 3/3 3/3 3/3
NGC 4826 3/ 3/ 3/
AGNs/QSOs
CenA 1/ 3/ 1/ 1/ *
3C273 2/2* 3/3
IZw1 2/2 3/3 3/3
Mrk 1014 3/3 3/3 3/3
NGC 1275 2/2 2/ 3/3 2/2*
3C120 /3 /3 /3
M87 2/2 3/3 3/3
Mrk 463 3/ 3/ 3/
Mrk 876 1613+658 /3 /3 /3
3C48 2/2*2/2*3/3
Edge-on
IC 2389 /2
UGC 5965 /3
UGC 9665 2/
UGC 11859 2/2
ESO12-1050 3/3
ESO480-0090 2/2
ESO157-0490 /3
* means line list modified for this source/instrument with respect to that
outlined for the various projects. For individual sources, these modifications
are:
SgrA* : 3.61HeH+, 3.953H3+, 4.695H2, 9.665H2, 16.331H3+, 39.399H2O added in
coordination with Drapatz et al. proposal
W51 IRS2: 3.235H2, 45.114H2O added in coordination with Drapatz et al. proposal
NGC 1068: 4.35H3+, 16.33H3+ added
NGC 891: only 4.052, 5.608, 8.991, 10.511, 12.279, 12.814, 14.320, 18.713,
25.913, 25.988, 28.219, 33.480, 34.814 will be observed
II Zw 40: 4.052H, 12.279H2, 25.988[FeII] added
NGC3690/IC694: 34.615 OH added
NGC 4945: 2.424H2, 5.511H2 added
NGC 5253: 4.052H, 12.279H2, 25.988[FeII] added
Mrk 231 : 34.615 OH added
Arp 220 : 34.615 OH added
NGC 6240: 4.35H3+, 16.33H3+ added
F10214+4724: See text above
13224-3809: 14.32NeV, 25.988[FeII] added
Cen A : no Mg, Si coronals except 3.935 and 5.608
3C273 : Only survey lines + 17.035H2, but deep integration
NGC 1275: no Mg, Si coronals except 3.935 and 5.608
3C48 : Modified due to redshift. Observed with SWS: 2.165H, 4.052H,
5.608[MgV], 6.985[ArII], 8.911[ArIII], 18.713[SIII], 25.913[OIV].
Observed with LWS: 33.480[SIII], 34.814[SiII], 63.184[OI]
<=== autumn_launch_targets ===>
1,"SWS01",1.,"N", "GC SgrA* ", 17.76112, -29.00794, 2000, 0., 0., 6498,0
2,"SWS02",2.,"N", "GC SgrA* ", 17.76112, -29.00794, 2000, 0., 0., 2694,0
3,"SWS01",1.,"N", "GC Ring NE ", 17.76161, -28.99725, 2000, 0., 0., 6498,0
4,"SWS02",2.,"N", "GC Ring NE ", 17.76161, -28.99725, 2000, 0., 0., 3346,0
5,"SWS01",1.,"N", "GC Ring SW ", 17.76073, -29.01825, 2000, 0., 0., 6498,0
6,"SWS02",2.,"N", "GC Ring SW ", 17.76073, -29.01825, 2000, 0., 0., 3346,0
7,"PHT40",3.,"N", "GC SgrA* ", 17.76112, -29.00794, 2000, 0., 0., 493,8
8,"PHT40",3.,"N", "GC Ring NE ", 17.76161, -28.99725, 2000, 0., 0., 333,9
9,"PHT40",3.,"N", "GC Ring SW ", 17.76073, -29.01825, 2000, 0., 0., 333,0
10,"SWS01",1.,"N", "RCW103 ion ", 16.29214, -51.10136, 2000, 0., 0., 6498,0
11,"PHT40",3.,"N", "RCW103 ion ", 16.29214, -51.10136, 2000, 0., 0., 493,0
12,"SWS01",1.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 6498,0
13,"SWS02",2.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 4402,0
14,"LWS01",2.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 570,0
15,"PHT40",3.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 493,0
16,"SWS01",1.,"N", "W 51 IRS2 ", 19.39443, +14.51835, 2000, 0., 0., 6498,0
17,"SWS02",2.,"N", "W 51 IRS2 ", 19.39443, +14.51835, 2000, 0., 0., 2580,0
18,"PHT40",3.,"N", "W 51 IRS2 ", 19.39443, +14.51835, 2000, 0., 0., 493,0
19,"SWS01",1.,"N", "M82 ", 9.93076, +69.67899, 2000, 0., 0., 6498,0
20,"SWS02",1.,"N", "M82 ", 9.93076, +69.67899, 2000, 0., 0., 2818,0
21,"PHT40",3.,"N", "M82 ", 9.93076, +69.67899, 2000, 0., 0., 493,0
22,"SWS01",2.,"N", "NGC 253 ", 0.79255, -25.28811, 2000, 0., 0., 6498,0
23,"SWS02",2.,"N", "NGC 253 ", 0.79255, -25.28811, 2000, 0., 0., 3258,0
24,"SWS02",2.,"N", "NGC 253 off ", 0.80013, -25.20350, 2000, 0., 0., 2112,0
25,"PHT40",3.,"N", "NGC 253 ", 0.79255, -25.28811, 2000, 0., 0., 493,0
26,"SWS01",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 6498,0
27,"SWS06",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 3985,0
28,"SWS06",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 6667,0
29,"SWS02",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 2112,0
30,"PHT40",3.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 493,0
31,"SWS01",1.,"N", "Circinus ", 14.21936, -65.33930, 2000, 0., 0., 6498,0
32,"SWS02",1.,"N", "Circinus ", 14.21936, -65.33930, 2000, 0., 0., 9180,0
33,"LWS01",1.,"N", "Circinus ", 14.21936, -65.33930, 2000, 0., 0., 570,0
34,"PHT40",3.,"N", "Circinus ", 14.21936, -65.33930, 2000, 0., 0., 493,0
35,"SWS01",1.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 6498,0
36,"SWS02",1.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 5902,0
37,"SWS02",1.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 8340,0
38,"PHT40",3.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 1261,0
39,"SWS02",1.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 7470,0
40,"SWS02",1.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 6036,0
41,"SWS02",2.,"N", "NGC 891 off ", 2.37652, +42.36697, 2000, 0., 0., 2112,0
42,"SWS02",2.,"N", "NGC 891 off1 ", 2.37706, +42.38028, 2000, 0., 0., 2112,0
43,"SWS02",2.,"N", "NGC 891 off2 ", 2.37759, +42.39581, 2000, 0., 0., 2112,0
44,"LWS01",2.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 960,0
45,"PHT40",3.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 1261,0
46,"SWS02",3.,"N", "NGC 4567 ", 12.60908, +11.25803, 2000, 0., 0., 2164,47
47,"SWS02",3.,"N", "NGC 4568 ", 12.60950, +11.24026, 2000, 0., 0., 948,0
48,"LWS01",3.,"N", "NGC 4567 ", 12.60908, +11.25803, 2000, 0., 0., 1740,49
49,"LWS01",3.,"N", "NGC 4568 ", 12.60950, +11.24026, 2000, 0., 0., 1580,0
50,"PHT40",3.,"N", "NGC 4567 ", 12.60908, +11.25803, 2000, 0., 0., 1261,51
51,"PHT40",3.,"N", "NGC 4568 ", 12.60950, +11.24026, 2000, 0., 0., 1101,0
52,"SWS02",3.,"N", "NGC 5194 M 51 ", 13.49797, +47.19515, 2000, 0., 0., 1108,0
53,"PHT40",3.,"N", "NGC 5194 M 51 ", 13.49797, +47.19515, 2000, 0., 0., 1261,0
54,"SWS02",3.,"N", "NGC 6052 ", 16.08692, +20.54215, 2000, 0., 0., 932,0
55,"SWS02",1.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 5898,0
56,"LWS01",1.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 960,0
57,"PHT40",3.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 1261,0
58,"SWS02",2.,"N", "NGC 3690 A ", 11.47601, +58.56293, 2000, 0., 0., 5576,0
59,"SWS02",2.,"N", "NGC 3690 A ", 11.47601, +58.56293, 2000, 0., 0., 4344,0
60,"SWS02",2.,"N", "NGC 3690 B/C ", 11.47524, +58.56266, 2000, 0., 0., 6364,0
61,"PHT40",3.,"N", "NGC 3690 A ", 11.47601, +58.56293, 2000, 0., 0., 1261,62
62,"PHT40",3.,"N", "NGC 3690 B/C ", 11.47524, +58.56266, 2000, 0., 0., 1101,0
63,"SWS02",1.,"N", "NGC 4945 ", 13.09095, -49.46819, 2000, 0., 0., 8186,0
64,"PHT40",3.,"N", "NGC 4945 ", 13.09095, -49.46819, 2000, 0., 0., 1261,0
65,"SWS02",3.,"N", "NGC 5236 M83 ", 13.61682, -29.86535, 2000, 0., 0., 8718,0
66,"SWS02",3.,"N", "NGC 5236 M83 ", 13.61682, -29.86535, 2000, 0., 0., 3904,0
67,"PHT40",3.,"N", "NGC 5236 M83 ", 13.61682, -29.86535, 2000, 0., 0., 1261,0
68,"SWS02",3.,"N", "NGC 4038 ", 12.03142, -18.86809, 2000, 0., 0., 756,69
69,"SWS02",3.,"N", "NGC 4039 ", 12.03148, -18.88614, 2000, 0., 0., 596,70
70,"SWS02",3.,"N", "NGC 4038/39 ov", 12.03192, -18.88448, 2000, 0., 0., 596,0
71,"PHT40",3.,"N", "NGC 4038 ", 12.03142, -18.86809, 2000, 0., 0., 1261,72
72,"PHT40",3.,"N", "NGC 4039 ", 12.03148, -18.88614, 2000, 0., 0., 1101,73
73,"PHT40",3.,"N", "NGC 4038/39 ov", 12.03192, -18.88448, 2000, 0., 0., 1101,0
74,"SWS02",3.,"N", "NGC 5253 ", 13.66548, -31.64140, 2000, 0., 0., 1978,0
75,"LWS01",3.,"N", "NGC 5253 ", 13.66548, -31.64140, 2000, 0., 0., 960,0
76,"PHT40",3.,"N", "NGC 5253 ", 13.66548, -31.64140, 2000, 0., 0., 1261,0
77,"SWS02",3.,"N", "F15564+6359 ", 15.95056, +63.84190, 2000, 0., 0., 6766,0
78,"LWS02",3.,"N", "F15564+6359 ", 15.95056, +63.84190, 2000, 0., 0., 640,0
79,"PHT40",3.,"N", "F15564+6359 ", 15.95056, +63.84190, 2000, 0., 0., 1261,0
80,"SWS02",3.,"N", "NGC 6764 ", 19.13788, +50.93319, 2000, 0., 0., 1222,0
81,"PHT40",3.,"N", "NGC 6764 ", 19.13788, +50.93319, 2000, 0., 0., 1261,0
82,"SWS02",3.,"N", "NGC 6946 ", 20.58120, +60.15385, 2000, 0., 0., 1512,0
83,"SWS02",3.,"N", "NGC 6946 off ", 20.58114, +60.21496, 2000, 0., 0., 2112,0
84,"SWS02",3.,"N", "NGC 6946 sky ", 20.58120, +60.35385, 2000, 0., 0., 1512,0
85,"PHT40",3.,"N", "NGC 6946 ", 20.58120, +60.15385, 2000, 0., 0., 1261,0
86,"SWS02",3.,"N", "NGC 7552 ", 23.26966, -42.58421, 2000, 0., 0., 756,0
87,"LWS01",3.,"N", "NGC 7552 ", 23.26966, -42.58421, 2000, 0., 0., 960,0
88,"PHT40",3.,"N", "NGC 7552 ", 23.26966, -42.58421, 2000, 0., 0., 1261,0
<=== spring_launch_targets ===>
1,"SWS01",1.,"N", "GC SgrA* ", 17.76112, -29.00794, 2000, 0., 0., 3498,0
2,"SWS01",1.,"N", "IC443 ion ", 6.29288, +22.88191, 2000, 0., 0., 6498,0
3,"PHT40",3.,"N", "IC443 ion ", 6.29288, +22.88191, 2000, 0., 0., 493,0
4,"SWS01",1.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 6498,0
5,"SWS02",2.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 4402,0
6,"LWS01",2.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 570,0
7,"PHT40",3.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 493,0
8,"SWS01",1.,"N", "DR 21 ", 20.65009, +42.32797, 2000, 0., 0., 6498,0
9,"SWS02",2.,"N", "DR 21 ", 20.65009, +42.32797, 2000, 0., 0., 5546,0
10,"LWS01",3.,"N", "DR 21 ", 20.65009, +42.32797, 2000, 0., 0., 570,0
11,"PHT40",3.,"N", "DR 21 ", 20.65009, +42.32797, 2000, 0., 0., 493,0
12,"SWS01",1.,"N", "M82 ", 9.93076, +69.67899, 2000, 0., 0., 6498,0
13,"SWS02",1.,"N", "M82 ", 9.93076, +69.67899, 2000, 0., 0., 2818,0
14,"PHT40",3.,"N", "M82 ", 9.93076, +69.67899, 2000, 0., 0., 493,0
15,"SWS01",2.,"N", "NGC 253 ", 0.79255, -25.28811, 2000, 0., 0., 6498,0
16,"SWS02",2.,"N", "NGC 253 ", 0.79255, -25.28811, 2000, 0., 0., 3258,0
17,"SWS02",2.,"N", "NGC 253 off ", 0.80013, -25.20350, 2000, 0., 0., 2112,0
18,"PHT40",3.,"N", "NGC 253 ", 0.79255, -25.28811, 2000, 0., 0., 493,0
19,"SWS01",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 6498,0
20,"SWS06",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0.,10352,0
21,"SWS02",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 2112,0
22,"PHT40",3.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 493,0
23,"SWS01",1.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 6498,0
24,"SWS02",1.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 5902,0
25,"SWS02",1.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 8340,0
26,"PHT40",3.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 1261,0
27,"SWS02",1.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 7470,0
28,"SWS02",1.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 6036,0
29,"SWS02",2.,"N", "NGC 891 off ", 2.37652, +42.36697, 2000, 0., 0., 2112,0
30,"SWS02",2.,"N", "NGC 891 off1 ", 2.37706, +42.38028, 2000, 0., 0., 2112,0
31,"SWS02",2.,"N", "NGC 891 off2 ", 2.37759, +42.39581, 2000, 0., 0., 2112,0
32,"PHT40",3.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 1261,0
33,"SWS02",3.,"N", "NGC 4567 ", 12.60908, +11.25803, 2000, 0., 0., 2164,34
34,"SWS02",3.,"N", "NGC 4568 ", 12.60950, +11.24026, 2000, 0., 0., 948,0
35,"LWS01",3.,"N", "NGC 4567 ", 12.60908, +11.25803, 2000, 0., 0., 1740,36
36,"LWS01",3.,"N", "NGC 4568 ", 12.60950, +11.24026, 2000, 0., 0., 1580,0
37,"PHT40",3.,"N", "NGC 4567 ", 12.60908, +11.25803, 2000, 0., 0., 1261,38
38,"PHT40",3.,"N", "NGC 4568 ", 12.60950, +11.24026, 2000, 0., 0., 1101,0
39,"SWS02",3.,"N", "NGC 5194 M 51 ", 13.49797, +47.19515, 2000, 0., 0., 1108,0
40,"PHT40",3.,"N", "NGC 5194 M 51 ", 13.49797, +47.19515, 2000, 0., 0., 1261,0
41,"SWS02",3.,"N", "II Zw 40 ", 5.92850, +03.39209, 2000, 0., 0., 4002,0
42,"SWS02",3.,"N", "He 2-10 ", 8.60416, -26.40941, 2000, 0., 0., 9330,0
43,"PHT40",3.,"N", "He 2-10 ", 8.60416, -26.40941, 2000, 0., 0., 1261,0
44,"SWS02",3.,"N", "IC 342 ", 3.78002, +68.09632, 2000, 0., 0., 5634,0
45,"SWS02",3.,"N", "IC 342 sky ", 3.78002, +68.19632, 2000, 0., 0., 5634,0
46,"PHT40",3.,"N", "IC 342 ", 3.78002, +68.09632, 2000, 0., 0., 1261,0
47,"SWS02",1.,"N", "NGC 1808 ", 5.12841, -37.51265, 2000, 0., 0., 5370,0
48,"LWS01",1.,"N", "NGC 1808 ", 5.12841, -37.51265, 2000, 0., 0., 960,0
49,"PHT40",3.,"N", "NGC 1808 ", 5.12841, -37.51265, 2000, 0., 0., 1261,0
50,"SWS01",1.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 6498,0
51,"SWS02",1.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 5898,0
52,"LWS01",1.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 960,0
53,"PHT40",3.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 1261,0
54,"SWS02",2.,"N", "NGC 3690 A ", 11.47601, +58.56293, 2000, 0., 0., 9740,0
55,"SWS02",2.,"N", "NGC 3690 B/C ", 11.47524, +58.56266, 2000, 0., 0., 6364,0
56,"PHT40",3.,"N", "NGC 3690 A ", 11.47601, +58.56293, 2000, 0., 0., 1261,57
57,"PHT40",3.,"N", "NGC 3690 B/C ", 11.47524, +58.56266, 2000, 0., 0., 1101,0
58,"SWS02",3.,"N", "NGC 1614 ", 4.56668, -08.57911, 2000, 0., 0., 756,0
59,"LWS01",3.,"N", "NGC 1614 ", 4.56668, -08.57911, 2000, 0., 0., 960,0
60,"PHT40",3.,"N", "NGC 1614 ", 4.56668, -08.57911, 2000, 0., 0., 1261,0
61,"SWS02",3.,"N", "NGC 2903 ", 9.53614, +21.50170, 2000, 0., 0., 756,0
62,"LWS01",3.,"N", "NGC 2903 ", 9.53614, +21.50170, 2000, 0., 0., 960,0
63,"PHT40",3.,"N", "NGC 2903 ", 9.53614, +21.50170, 2000, 0., 0., 1261,0
64,"SWS02",2.,"N", "NGC 3079 ", 10.03272, +55.67995, 2000, 0., 0., 1864,0
65,"SWS02",2.,"N", "NGC 3079 off ", 10.03409, +55.65462, 2000, 0., 0., 2112,0
66,"LWS01",2.,"N", "NGC 3079 ", 10.03272, +55.67995, 2000, 0., 0., 960,0
67,"PHT40",3.,"N", "NGC 3079 ", 10.03272, +55.67995, 2000, 0., 0., 1261,0
68,"SWS02",3.,"N", "NGC 4038 ", 12.03142, -18.86809, 2000, 0., 0., 756,69
69,"SWS02",3.,"N", "NGC 4039 ", 12.03148, -18.88614, 2000, 0., 0., 596,70
70,"SWS02",3.,"N", "NGC 4038/39 ov", 12.03192, -18.88448, 2000, 0., 0., 596,0
71,"PHT40",3.,"N", "NGC 4038 ", 12.03142, -18.86809, 2000, 0., 0., 1261,72
72,"PHT40",3.,"N", "NGC 4039 ", 12.03148, -18.88614, 2000, 0., 0., 1101,73
73,"PHT40",3.,"N", "NGC 4038/39 ov", 12.03192, -18.88448, 2000, 0., 0., 1101,0
74,"SWS02",3.,"N", "NGC 6764 ", 19.13788, +50.93319, 2000, 0., 0., 1222,0
75,"PHT40",3.,"N", "NGC 6764 ", 19.13788, +50.93319, 2000, 0., 0., 1261,0
76,"SWS02",3.,"N", "NGC 6946 ", 20.58120, +60.15385, 2000, 0., 0., 1512,0
77,"SWS02",3.,"N", "NGC 6946 off ", 20.58114, +60.21496, 2000, 0., 0., 2112,0
78,"SWS02",3.,"N", "NGC 6946 sky ", 20.58120, +60.35385, 2000, 0., 0., 1512,0
79,"LWS01",3.,"N", "NGC 6946 ", 20.58120, +60.15385, 2000, 0., 0., 960,0
80,"PHT40",3.,"N", "NGC 6946 ", 20.58120, +60.15385, 2000, 0., 0., 1261,0
81,"SWS02",3.,"N", "NGC 7552 ", 23.26966, -42.58421, 2000, 0., 0., 5898,0
82,"LWS01",3.,"N", "NGC 7552 ", 23.26966, -42.58421, 2000, 0., 0., 960,0
83,"PHT40",3.,"N", "NGC 7552 ", 23.26966, -42.58421, 2000, 0., 0., 1261,0