<=== observer ===>
"CTELESCO",\
"Telesco, C. M.",\
"Space Science Laboratory",\
"NASA Marshall Space Flight Center",\
"",\
"Mail Code ES-63",\
"",\
"Huntsville AL 35812",\
"USA",\
"0010205 5447723",\
"0010205 5447754",\
"telesco@ssl.msfc.nasa.gov"
<=== proposal ===>
"HI_Z_PT1",1,4,\
{"starburst galaxies","galaxy formation","irregular galaxies"},\
{"U. Klaas","A. Moorwood","H. Hippelein"}
<=== title ===>
Blue Radio Galaxies at Intermediate Redshifts:
Part 1
<=== abstract ===>
SCIENTIFIC ABSTRACT
We propose to use ISOPHOT at 24, 64, and 100 um and ISOCAM at 15 um to study
galaxies at z > 0.1 which, based on their blue colors, are thought to be
undergoing bursts of star formation. Most of these galaxies were discovered
as radio sources in the deep 1.4 GHz surveys. Many have complex optical
morphologies suggesting that they are interacting and merging systems,
although other explanations such as jet-induced star formation have been put
forward. These galaxies are thought to account for the excess, or "upturn,"
in the 1.4 GHz radio source counts detected at flux densities below a few
milliJanskys. Our study will show if there exist significant obscured
populations of young stars in these galaxies, and it will substantially extend
our knowledge of the population of IR-luminous galaxies to the realm at z >
0.1 and possibly out to z = 1-2. The total luminosities and dust color
temperatures will be determined from the fluxes at 64 and 100 um, where the
spectral energy distributions peak. The 15, 24, and 64 um fluxes may indicate
the presence of active nuclei which produce a peak in this spectral region in
several local Seyfert archetypes.
OBSERVATION SUMMARY
We propose to observe 51 galaxies for an Autumn launch (exclusion hole in
Orion) or 58 galaxies for a Spring launch (exclusion hole in the Galactic
Center), most at 24, 64, and 100 um with PHOT and at 15 um with CAM, for a
total spacecraft time of 17 hours. Five hours of this spacecraft time have
been contributed by Mission Scientist Alan Moorwood. Most of the sources have
1.4 GHz flux densities of a few mJy, with expected 60 um flux densities of
greater than 100 mJy if the radio-infrared relation for local galaxies applies
to these distant ones. Each of these brighter galaxies will be observed using
PHT filters C100, C60, and P25 and CAM filter LW3. A smaller sample of
fainter galaxies, with expected 60 um flux densities greater than 30 mJy will
be observed only with C100, C60, and LW3. The PHOT observations will employ
triangular chopping, and the CAM imaging will use 2x2 microscans. Because
these galaxies are grouped in several small regions of the sky, we propose to
use concatenation to substantially reduce overhead. In addition to the purely
scientific reasons mentioned in the abstract, the CAM images will verify
telescope pointing and aid in the assessment of cirrus contamination at the
longer wavelengths.
<=== scientific_justification ===>
Time table includes times of parts 1 and 2!
Time distribution for autumn launch targets
Team top 40% second 30% last 30%
PHT : 14534 15805 15316
AFM : 10800 0 7200
total : 25334 15805 22516
Time distribution for spring launch targets
Team top 40% second 30% last 30%
PHT : 15435 20294 9771
AFM : 10800 0 7200
total : 26235 20294 16971
WHAT IS KNOWN?
Astronomers are striving to formulate a comprehensive description of the
evolution of galaxies. A key element of this quest is the search for, and
detailed study of, galaxies at great distances. By examining galaxies as a
function of redshift, and hence lookback time, we should be able to piece
together the scenario that has led to the currently observed Universe. The
actual discovery of distant galaxies (i.e., those at z > 0.1) is difficult and
challenging. Deep surveys at radio wavelengths followed by visual imaging and
spectroscopy of the radio sources has proven to be very effective for finding
distant galaxies. With this approach, galaxies have been discovered at z > 2.
Many of these radio galaxies appear to be giant ellipticals undergoing
"passive" stellar evolution, defined as the normal aging of the previously
formed dominant stellar population (Lilly and Longair 1984; Kron, Koo, and
Windhorst 1985). However, as one considers progressively fainter radio fluxes
and higher redshifts, one finds that an increasingly larger fraction of these
galaxies are very blue and are evidently experiencing intense star formation;
blue radio galaxies constitute one-third of the radio sample at flux densities
S(1.4 GHz) * 10 mJy, but over two-thirds of the sample at S(1.4 GHZ) < 3 mJy
(Windhorst et al. 1985). These blue galaxies appear to be the excess
population of 1.4 GHz radio sources discovered by Windhorst et al.(1985) at
flux densities less than 5 mJy; this excess is also apparent at 4.86 and 8.44
GHz (see Windhorst et al. 1993). Known populations of Seyfert and spiral
galaxies or simply evolving populations of ellipticals or quasars cannot
account for this "upturn" in the differential source counts. Imaging of many
of the sources (Kron et al. 1985) indicates that they are morphologically
complex, which, with their blue colors, strongly suggests that they are
interacting or merging systems undergoing luminous bursts of star formation;
an alternative possiblity is that the star formation has been induced by the
passage of a plasma jet through the interstellar medium (e.g., Miley et al.
1992). Visual spectroscopy often shows the narrow emission lines expected
from starburst HII regions. The maximum redshift measured thus far for blue
galaxies in this sample (and available in the literature) is 0.4, which
corresponds roughly to 30% of the Hubble time and is cosmologically
significant. Windhorst and colleagues and others (e.g., Benn et al. 1993) are
continuing to measure redshifts of visually fainter, and therefore possibly
more distant, blue radio galaxies. Currently the faintest blue radio galaxies
have F = 23 mags, which, based on the redshifts available for the brighter
galaxies, may correspond to z = 1 (Donnelly, Partridge, and Windhorst 1987).
However, recent redshift determinations for some of these fainter galaxies
imply that many, or even most, of them may be at z < 1 and that they may
therefore be a hitherto unknown population of lower-luminosity blue galaxies
which do not exist in significant numbers in the local universe (Cowie et al.
1991). In either case, it is clear that the far-IR detection of these very
faint blue radio galaxies would be a major advance in our knowledge of
galactic luminosity evolution. We propose to study them with ISOPHOT and
ISOCAM.
OPEN PROBLEMS
The broad range of issues relevant to our proposal concerning the evolution of
galaxies include the following. (1) Were interactions in the past more
effective at initiating bursts of star formation than interactions are now? A
greater star formation rate in a younger galaxy might result from there being
a larger gas content. A greater number of interactions and starbursts may
have resulted from there being a greater number of galaxies per unit volume, a
conclusion consistent with the upturn in the radio-galaxy source counts
mentioned above. An important related issue is whether the "ultraluminous"
galaxies, with L(IR)>10**12 L(sun), are more common at higher z.(2) Was the
dust content in galaxies different at epochs out to z = 1? This question bears
strongly on the relationship of galactic dust content to metallicity and to
the efficiency and rate of star formation which depends critically on the
elemental and dust abundances. A very low IR luminosity in a very blue galaxy
with other hallmarks of a recent starburst may betoken a galaxy deficient in
dust. (3) Does the nature of blue galaxies change with increasing lookback
time? Such changes might be manifested as variations with z in the
IR-to-visual luminosity ratio, IR color temperature, and, of course, the IR
luminosity. (4) If the faint blue radio galaxies are relatively nearby (i.e.,
at z = 0.2-0.4), what is their relationship to galaxies in the local Universe?
(5) What are the relative roles of young stars and active nuclei (i.e., black
holes) in the generation of the luminosity? (6) If the extended radio and
visual emission results from jet-induced star formation (Miley et al. 1992),
does the "efficiency" of that star formation differ significantly from that
generated by other mechanisms such as bars and spiral arms?
WHY ISO?
We know nothing about the IR luminosity (and hence the bolometric luminosity,
much of which emerges in the IR) of galaxies at z > 0.1, i.e., outside the
local Universe. The determination of the far-IR luminosities of distant
galaxies is the primary goal of this proposal. ISO will be the only
observatory until SIRTF with the sensitivity to carry out these observations.
We have chosen as our sample the blue galaxies from the radio surveys by
Windhorst and colleagues and Mitchell & Condon (1985) because radio galaxies
that are blue are more likely to emit in the far-IR; based on IRAS studies,
the galaxies that are the most IR-luminous tend to be both bluer and have
higher IR-to-blue ratios than average (e.g. Bothun, Lonsdale, and Rice 1989).
Starburst and Seyfert galaxies are the most outstanding examples.
We consider the sensitivity of the relevant PHOT and CAM passbands to galaxies
with IR luminosities in the range (0.03-1.5)x10**12 L(sun) and with spectral
energy distributions (SEDs) like those of the nearby (3.3 Mpc) starburst
galaxy M82 and the more distant (z = 0.018) ultraluminous AGN/starburst galaxy
Arp 220. We find that a galaxy like M82, which emits 3x10**10 L(sun) and is not
unusually luminous, should be easily detected out to z = 0.2 in all the
relevant passbands after only 100 sec of integration. For the same
int. time, a galaxy emitting 1.5x10**12 L(sun) could be detected out to z >
1 at 100 um and out to z > 0.5 at 64 um. Galaxies as bright as Markarian 231,
with LIR = 3x10**12 L(sun), will be detectable at 100 um out to z = 1.5. We
conclude that ISO, and only ISO, will be able to detect the IR emission of
luminous galaxies out to cosmologically interesting redshifts of z > 0.2 and
possibly as high as z = 1.5.
The most important single piece of data we hope to get from our proposed
observations on each galaxy is the IR luminosity LIR, most of which is emitted
longward of 40 um in most galaxies. Therefore, we emphasize observations at
64 and 100 um. Using this derived LIR for each galaxy we will be able to
estimate star formation rates, and we will be able to determine where the IR
emission from this sample of galaxies fits into the continuum of IR activity
observed in galaxies in the local Universe. We will be able to determine to
first order if starbursts resulting from galaxy interactions and mergers were
different in the past; were they more effective or efficient at producing
stars? Are these blue galaxies a unique population essentially different from
nearby galaxies? For those galaxies for which we can obtain reliable data at
both 64 and 100 um, dust color temperatures can be estimated. The
characteristic dust temperature is a very useful auxiliary diagnostic, since
it indicates, as a complement to LIR, the intensity of the starburst, with a
higher color temperature implying a higher average energy density for the UV
radiation that heats the dust (e.g., Telesco, Wolstencroft, and Done 1988).
The IR colors can also help us distinguish between starburst-powered and
AGN-powered IR luminosity, since there is a strong tendency for AGN-powered IR
emission to exhibit a broad bump in the 10-30 um spectral region, as
exemplified by the Seyfert/starburst galaxy NGC 1068 (Telesco et al.1984;
Telesco and Harper 1980). Therefore, in addition to the 60 and 100 um
observations proposed above for PHOT, we propose to observe each galaxy at 24
um using PHT and at 15 um using CAM. Excess 10-to-30 um emission due to the
presence of an AGN should be manifested by a bluer 15 um-24 um and 24 um-60 um
colors. Imaging with CAM will also have the substantial added advantage that
we can verify the telescope pointing, since the galaxy will be a point source
clearly evident in the CAM images. Furthermore, because we have a rough idea
of the IR spectral energy distributions expected from galaxies, we can
extrapolate to longer wavelengths from the 15 and 24 um fluxes detected to
estimate the far-IR flux density and thereby assess the contribution of local
cirrus emission to the detected far-IR flux; the effectiveness of the PHOT
chopping in the removal of the cirrus background will depend on the cirrus
spatial structure on scales not yet studied.
WHAT GROUNDBASED/AIRBORNE OBSERVATIONS ARE LIKELY BEFORE ISO
This project is not possible with any instrument other than ISO. However,
observations of nearby galaxies with the Kuiper Airborne Observatory (for
which the best far-IR sensitivity is about 1 Jy, S/N=4 in 1 hour of
integration) and further analysis of the IRAS data will provide considerable
information necessary for the interpretation of the PHOT and CAM observations
of distant galaxies. The major impact of technological developments prior to
the ISO launch will be that significantly more of the blue galaxies in our
proposed sample will have had their redshifts determined.
OBSERVING STRATEGY
We propose to observe each galaxy first with the two PHT-C100 passbands and
one PHT-P2: 64 um (C-60), 100 um (C-100), and 23.9 um (P-25). The longer-
wavelength passbands have excellent sensitivity, and they span the spectral
region of maximum emission thereby providing the most reliable estimate of
LIR. Detection at 64 and 100 um also has the substantial advantage of
permitting a convenient comparison of our results to the large body of IRAS
observations of galaxies at those wavelengths. The PHT observation of each
galaxy will be followed by observations in the CAM LW3 filter which has a
central wavelength of 15 um (although the effective wavelength will be longer
because the passband is wide and the spectral energy distributions of these
galaxies should be steeply rising toward longer wavelengths). The pixel size
for the CAM imaging will be 3".
Because of the original radio discovery strategy for these sources, the
galaxies in our sample are grouped in certain regions of the sky. Therefore,
for convenience in planning and assessment, we have explicitely indicated each
group with a field designation A, B, C, D (1 or 2), and E depending on the
location. The galaxies that we propose to observe are listed in Tables 1 and
2 for each of the major fields. The first 64 entries in Table 1 (fields A, B,
C, and D1) constitute all of the blue galaxies (J-F<1.2 for F<18, and J-F<
0.2F-2.4 for F>18) discovered in the 1.4 GHz radio survey at Westerbork (WBK)
by Windhorst, van Heerde, and Katgert (1984) and for which imaging was
obtained by Windhorst and colleagues (Windhorst, Kron, and Koo 1984; Kron,
Koo, and Windhorst 1985). The optical J and F bands to which we refer here
correspond approximately to 4650 A and 6100 A, respectively. The last 9
entries in Table 1 (field D2) were discovered by Windhorst et al.(1985) in the
deep 1.4 GHz VLA study of one of the Westerbork fields; we will observe only
those with 1.4 GHz flux densities greater than 0.4 mJy. Redshifts have been
measured for 21 of the 58 sources in Table 1. Many additional redshifts will
have been obtained for this sample prior to the ISO mission, with all of them
being measured eventually. Very accurate positions are available from both
radio and visual imaging of the blue galaxies that we propose to observe with
ISO; the optical positions are presented in Table 1.
The 12 objects listed in Table 2 (field E) are all of those designated
starburst galaxies by Benn et al. (1993) and which are located in neither the
Orion hole nor the Galactic Center hole. The starburst designations for these
objects are based on optical spectroscopy of optical identifications of
sources from the deep 1.4 GHz surveys by Mitchell & Condon (1985). Redshifts
are available for all of these objects.
To facilitate planning, we can predict 60 um flux densities for our program
galaxies by assuming that the radio-IR relation that holds for nearby
starburst galaxies also holds for our sample: F(60um)/S(1.4GHz) = 100 (e.g.,
Condon 1987), where F and S are the flux densities at 60 um and 1.4 GHz,
respectively. The 1.4 GHz flux densities for the 64 galaxies in Fields A, B,
C, and D1 are typically a few mJy. The radio-IR relation then suggests that
the typical 60 um flux density for that sample will be a few hundred mJy. The
radio flux densities for the 21 galaxies in fields D2 and E are much lower
than those for other sample galaxies; the blue galaxies in fields D2 and E
will have typical 60 um flux densities of several tens of mJy. We emphasize
that these estimates are very uncertain, both because there is actually a
large spread in the radio-IR ratio for nearby galaxies and because we do not
know if the "canonical" relation is appropriate for the distant blue galaxies.
Table 1. Sample of Blue Galaxies Selected from Windhorst et al.
_______________________________________________________________________________
Name RA(1950) Dec(1950) z F J-F S(21 cm)
H M S D M S mag mag mJy
_______________________________________________________________________________
FIELD A
52W005 13 04 27.44 29 31 17.4 21.44 1.74 7.75
008 13 05 00.65 29 18 26.6 21.92 0.40 20.49
012 13 05 23.81 29 19 02.9 0.400 22.11 0.99 10.02
017 13 05 42.03 29 35 42.2 22.49 1.55 4.09
020 13 05 57.51 30 00 01.8 0.060 16.53 1.06 3.06
022 13 06 10.56 29 50 19.6 22.95 0.78 4.16
023 13 06 11.55 29 42 26.3 0.202 19.65 0.40 1.22
034 13 06 45.50 29 30 03.8 20.50 0.77 1.93
037 13 06 53.39 29 38 00.7 0.023 15.14 0.44 4.77
FIELD B
53W005 17 13 22.37 50 31 42.8 22.82 1.03 7.58
011 17 13 50.23 49 59 03.5 20 72 1.41 3.48
025 17 15 07.87 50 20 11.3 22.68 0.88 1.14
026 17 15 12.12 49 50 24.0 21.32 1.60 21.10
027 17 15 12.12 50 27 06.8 22.00 1.08 8.25
034 17 15 38.94 50 03 44.3 21.96 0.89 10.93
035 17 15 41.04 50 21 49.6 21.94 1.76 4.39
058 17 18 03.28 50 00 41.4 0.034 15.61 1.13 1.39
062 17 18 16.62 50 02 05.2 21.39 1.77 1.74
065 17 18 24.37 50 00 37.6 21.94 0.96 5.25
068 17 18 43.28 49 39 06.2 22.98 -0.18 3.89
071 17 18 56.89 50 20 13.2 20.90 1.08 2.78
072 17 19 15.28 50 25 32.5 15.09 1.17 6.56
083 17 20 33.81 50 05 28.9 22.02 1.12 5.02
090 17 21 08.67 49 59 30.3 0.094 16.90 0.67 2.06
FIELD C
54W008 00 13 16.40 15 48 42.3 0.015 14.00 0.75 12.08
013 00 13 39.76 16 11 28.6 0.249 17.99 0.58 1.51
018 00 13 49.84 15 53 30.4 0.038 17.08 0.82 3.22
034 00 14 20.62 16 07 05.3 17.24 0.70 2.10
036 00 14 26.15 15 22 53.5 21.27 1.03 5.72
050 00 15 00.34 15 12 47.8 22.75 0.82 17.58
54W052 00 15 05.71 15 54 26.3 22.24 0.77 10.40
053 00 15 06.13 15 30 55.8 0.302 20.63 0.69 2.82
057 00 15 09.52 16 34 36.8 23.07 -0.02 476.60
065 00 15 31.71 16 19 16.0 23.06 0.40 2.55
067 00 15 34.92 16 20 52.7 22.16 0.29 66.55
068 00 15 35.01 16 32 52.7 22.57 1.63 24.61
071 00 15 41.66 16 29 37.0 0.287 22.28 1.12 5.41
072 00 15 42.29 16 26 45.1 19.10 1.01 2.77
54W081 00 16 01.89 15 41 50.7 19.87 1.05 15.02
FIELD D1
55W010 08 32 49.42 45 07 47.8 19.15 1.16 32.76
020 08 33 42.19 45 20 22.8 0.040 14.72 0.96 2.37
027 08 33 55.75 45 09 00.9 22.07 0.86 1.83
034 08 34 09.00 45 35 50.8 22.76 0.40 4.19
036 08 34 15.56 45 15 46.3 20.41 1.55 6.29
049 08 35 35.89 44 50 52.4 20.76 1.53 4.52
066 08 36 52.06 45 16 17.1 21.18 1.28 24.70
077 08 37 30.48 44 45 18.7 0.126 17.47 1.11 8.75
097 08 38 30.27 44 53 59.1 19.86 1.37 0.91
102 08 38 46.87 45 04 52.9 23.00 -0.05 9.66
135 08 41 17.73 44 32 31.2 0.089 16.25 0.86 2.38
137 08 41 22.84 44 55 32.2 0.160 17.80 0.90 1.60
144 08 41 53.92 45 12 11.2 20.38 1.02 2.68
150 08 42 05.38 45 01 34.1 20.73 1.38 0.84
153 08 42 08.31 45 07 08.3 22.33 0.83 1.94
158 08 42 41.19 44 41 52.6 20.35 1.15 0.69
171 08 43 43.31 44 33 46.9 20.68 1.29 2.89
175 08 44 10.58 44 15 13.2 21.74 0.86 42.90
178 08 44 21.05 44 45 52.6 0.041 15.49 0.92 1.24
183 08 44 37.71 44 44 10.0 0.088 19.32 0.64 1.33
184 08 44 39.48 44 39 35.0 21.92 1.34 1.07
188 08 45 03.00 44 52 35.2 22.13 1.36 12.10
191 08 45 16.35 44 13 04.4 21.68 1.19 13.99
199 08 45 42.90 44 32 28.9 22.40 0.74 3.36
226 08 47 35.74 44 34 40.3 20.83 1.49 6.35
FIELD D2
0839+44.03 08 39 55.17 44 43 27.6 17.13 1.10 1.05
0840+44.02 08 40 08.98 44 57 28.2 21.58 1.63 0.91
0840+45.02 08 40 40.33 45 00 27.7 22.19 0.81 0.59
0841+44.10 08 41 11.00 44 59 53.4 21.53 1.39 0.48
0841+44.15 08 41 18.47 44 56 27.2 0.147 17.14 1.00 0.80
0841+44.28 08 41 41.37 44 52 01.4 21.30 1.49 0.98
0841+45.03 08 41 49.64 45 04 04.0 21.46 1.53 0.63
0842+44.12 08 42 39.70 44 40 08.0 20.90 1.44 0.60
0843+44.07 08 43 16.43 44 44 46.0 0.125 17.69 1.13 0.67
_____________________________________________________________________________
Table 2. Sample of Blue Radio Galaxies Selected
from Benn et al. (1993)
_____________________________________________________________________________
Name RA(1950) Dec(1950) z B S(21 cm)
H M S D M S mag mJy
_____________________________________________________________________________
FIELD E
M003 12 59 05.53 30 41 08.0 0.1076 16.5 2.90
M015 12 59 39.11 30 43 38.8 0.0623 14.0 0.45
M022 12 59 47.32 30 46 32.1 0.3389 21.0 0.56
M028 12 59 54.00 30 42 54.0 0.1620 19.0 0.15
M043 13 00 12.49 30 27 40.7 0.0452 16.5 0.30
M049 13 00 16.70 30 34 31.2 0.2445 21.1 0.32
M051 13 00 17.61 30 33 46.5 0.1700 19.5 0.26
M056 13 00 22.43 30 47 26.6 0.2907 21.5 0.37
M063 13 00 27.73 30 26 55.7 0.1710 19.5 0.24
M064 13 00 27.83 30 34 22.3 0.1697 19.0 0.25
M097 13 00 55.71 30 17 38.2 0.2350 18.5 0.41
M141 13 01 57.15 30 36 17.5 0.3109 19.0 0.52
_______ ________________________________________________________________
We propose to observe the blue radio galaxies in the sample described above
down to 1 sigma noise levels of approximately 1-5 mJy at 25, 64, and 100 um and
0.1-0.2 mJy at 15 um. The faintest sources (fields E and D2) will only be
observed at 15, 64, and 100 um. These sensitivities should permit us to
detect the blue radio galaxies with S/N > 5 in these passbands even if the
radio-IR relation for these galaxies differs significantly from that
applicable to nearby galaxies. The PHOT observations will be made with PHT-P2
filter P-25 and with PHT-C100 filters C-60 and C-100. The CAM observations
will be made with filter LW3. All observations will be at a single position
(the central pixel centered on the object's nominal position), and triangular
chopping will be required for the PHOT observations.
Because we must plan for the launch of ISO to be in either the Autumn or the
Spring, we must have two lists of objects, one for each launch window. The
objects must not be located in the exclusion regions ("holes") for either
launch window. By grouping our objects into fields (see Tables 1 and 2), it
is easy for us to designate the object lists appropriate for either launch
period. Thus, the 51 objects we will observe for an Autumn launch are all of
those in fields A, B, C, and E, none of which falls in the Orion hole. The 58
objects we will observe for a Spring launch are all of those in fields A, C,
and D (i.e., D1 and D2), none of which falls in the Galactic Center hole.
Because the total number of objects (as well as the relative number of radio-
brighter ones and radio-fainter ones) is somewhat different for the two launch
windows, the total integration times are somewhat different for the two launch
possibilities. The observations are summarized in Table 3.
Table 3: Summary of Proposed Observations
________________________________________________________________________________
Detector Filter Lambda tint(s) F(mJy) Sub-sample tint(h)
Assembly (um) On source S/N=1 Fields On source
Each object Each sub-sample
_________________________________________________________________
AUTUMN LAUNCH (ORION HOLE)
PHT-C100 C100 100 128 2.9 A+B+C (39) 1.39
256 2.1 E(12) 0.85
PHT-C100 C60 64 128 4.0 A+B+C (39) 1.39
512 2.0 E (12) 1.71
PHT-P2 P25 23.9 64 1.1 A+B+C (39) 0.69
CAM LW3 15 120 0.2 A+B+C (39) 1.30
154 0.2 E (12) 0.51
SPRING LAUNCH (GALACTIC CENTER HOLE)
PHT-C100 C100 100 128 2.9 A+C+D1 (49) 1.74
256 2.1 D2 (9) 1.14
PHT-C100 C60 64 128 4.0 A+C+D1 (49) 1.74
256 2.8 D2 (9) 1.14
PHT-P2 P25 23.9 64 1.1 A+C+D1 (49) 0.87
CAM LW3 15 120 0.2 A+C+D1 (49) 1.63
120 0.2 D2 (9) 0.30
_______________________________________________________________________
Two additional considerations must be mentioned. First, there is currently
(as of 1 November 1993) significant ambiguity about the in-orbit performance
to be expected for the PHT-P detectors; the P2 detector could be less
sensitive by nearly an order of magnitude than the nominal values. If that P2
degradation is verified, we propose to eliminate the planned P2 observations
and: (1) double the C100 (100 um) integration time to 512 sec for each object
in field E for the Autumn launch; (2) double the C60 (64 um) integration time
to 512 sec for the faintest (at radio wavelengths) 8 objects in the field D2.
These changes will leave the total integration time virtually unchanged.
The total required integration time can be determined by referring to Table 3.
The on-source integration time is the summation of the numbers, designated
tint(hours), in the last column. For an Autumn launch these are 6.03 hours
for the PHOT observations and 1.81 hours for the CAM observations, but since
the PHOT observations require triangular chopping, the actual Autumn-launch
integration time will be (2 x 6.03) + 1.81 = 13.87 hours. For a Spring launch
the on-source integration times are 6.63 hours for the PHOT observations and
1.93 hours for the CAM observations. With triangular chopping for the PHOT
observations, the total Autumn-launch integration time is (2 x 6.63) + 1.93 =
15.19 hours. Note that Mission Scientist Alan Moorwood is contributing 5
hours of his spacecraft time for this project.
For completeness, we show in Table 4 the values for the background fluxes and
both cirrus and galaxy confusion for the fields considered in this proposal.
These values were computed for us by Dr. Steven Lord of the Infrared
Processing and Analysis Center (IPAC). The calculations assume aperture sizes
of 52" circular at 25 um and 44" x 44" (square pixel) at 60 and 100 um.
Chopping is triangular, with the throw being 52" at 25 um and 44" at 60 and
100 um. The galaxy confusion limits are the same for all fields. It should be
noted that the C100 chopping means that we actually integrate twice as long on
the source as we have previously indicated, since the source chops from one-
pixel to the adjacent one during the chop cycle; however, because of
uncertainties in the expected system performance, we do not alter our
integration requirements as a result of this special procedure. In addition,
such a short chopper throw may not be permitted by the AOTs.
Table 4. Background and Confusion Estimates
_________________________________________________________________
Field Background (mJy) Cirrus Confusion (mJy)
25 60 100 25 60 100
_________________________________________________________________
A 2000 630 380 Not Available
B 1215 370 350 0.3-0.8 0.01-0.04 0.03-0.09
C 2800 1000 600 1.7-6.4 0.8-3.0 2.0-7.0
D 2300 760 460 0.4-1.4 0.2-0.7 0.4 -1.6
E 1950 620 380 Not Available
Galaxy Confusion: 0.1-0.3 0.9-1.3 2.7-4.2
_________________________________________________________________
OTHER ISO OBSERVATIONS
Several proposals are complementary and will be useful for the full
realization of our scientific goals. Using ISOPHOT, Klaas et al. have
proposed to observe the IR energy distributions of the most luminous
ultraluminous. Many of those galaxies are relatively nearby (compared to our
sample) and will serve as archetypes for the interpretation of our
observations of distant blue galaxies. Likewise, the proposal to observe a
"core" galaxy sample (Joseph et al.) and a Virgo Cluster sample (Volk et al.)
will provide important comparison samples. Finally, Chase et al. have
proposed to use ISOCAM to image several distant clusters; the objects they
will observe may be similar to those in our proposed sample; at present we do
not know if our program galaxies are in clusters. Cross pollination between
our proposal and that by Chase et al. will be essential.
REFERENCES
Ackermann 1990, Confusion Limits for ISOPHOT
Benn et al. 1993, MNRAS, 263, 98
Bothun, Lonsdale, & Rice 1989, ApJ, 341, 129
Condon 1987, in Starbursts and Galaxy Evolution, p.425
Cowie, Songaila, & Hu 1991, Nature, 354, 460
Donnelly, Partridge, & Windhorst 1987, ApJ, 321, 94
Kron, Koo, & Windhorst 1985, A&A, 146, 38
Lilly and Longair 1984, MNRAS, 211, 833
Miley et al. 1992, ApJL, 401, L69
Mitchell & Condon 1985, AJ, 90, 1957
Telesco et al. 1984, ApJ, 282, 427
Telesco & Harper 1980, ApJ, 235, 392
Telesco, Wolstencroft, & Done 1988, ApJ, 329, 174
Windhorst et al. 1993, ApJ, 405, 498
Windhorst et al. 1985, ApJ, 289, 494
Windhorst, van Heerde, & Katgert 1984, A&AS, 58, 1
Windhorst, Kron, & Koo 1984, A&AS, 58, 393
<=== autumn_launch_targets ===>
1, "PHT22", 1.0, "N", "52W005", 13.07429, 29.52150, 1950, 0., 0., 817, 2
2, "PHT03", 1.0, "N", "52W005", 13.07429, 29.52150, 1950, 0., 0., 238, 3
3, "CAM01", 1.0, "N", "52W005", 13.07429, 29.52150, 1950, 0., 0., 148, 4
4, "PHT22", 1.0, "N", "52W008", 13.08351, 29.30739, 1950, 0., 0., 657, 5
5, "PHT03", 1.0, "N", "52W008", 13.08351, 29.30739, 1950, 0., 0., 238, 6
6, "CAM01", 1.0, "N", "52W008", 13.08351, 29.30739, 1950, 0., 0., 148, 7
7, "PHT22", 1.0, "N", "52W012", 13.08995, 29.31747, 1950, 0., 0., 657, 8
8, "PHT03", 1.0, "N", "52W012", 13.08995, 29.31747, 1950, 0., 0., 238, 9
9, "CAM01", 1.0, "N", "52W012", 13.08995, 29.31747, 1950, 0., 0., 148, 10
10, "PHT22", 1.0, "N", "52W017", 13.09501, 29.59506, 1950, 0., 0., 657, 11
11, "PHT03", 1.0, "N", "52W017", 13.09501, 29.59506, 1950, 0., 0., 238, 12
12, "CAM01", 1.0, "N", "52W017", 13.09501, 29.59506, 1950, 0., 0., 148, 13
13, "PHT22", 1.0, "N", "52W020", 13.09931, 30.00050, 1950, 0., 0., 657, 14
14, "PHT03", 1.0, "N", "52W020", 13.09931, 30.00050, 1950, 0., 0., 238, 15
15, "CAM01", 1.0, "N", "52W020", 13.09931, 30.00050, 1950, 0., 0., 148, 16
16, "PHT22", 1.0, "N", "52W022", 13.10293, 29.83878, 1950, 0., 0., 657, 17
17, "PHT03", 1.0, "N", "52W022", 13.10293, 29.83878, 1950, 0., 0., 238, 18
18, "CAM01", 1.0, "N", "52W022", 13.10293, 29.83878, 1950, 0., 0., 148, 19
19, "PHT22", 1.0, "N", "52W023", 13.10321, 29.70731, 1950, 0., 0., 657, 20
20, "PHT03", 1.0, "N", "52W023", 13.10321, 29.70731, 1950, 0., 0., 238, 21
21, "CAM01", 1.0, "N", "52W023", 13.10321, 29.70731, 1950, 0., 0., 148, 22
22, "PHT22", 1.0, "N", "52W034", 13.11264, 29.50106, 1950, 0., 0., 657, 23
23, "PHT03", 1.0, "N", "52W034", 13.11264, 29.50106, 1950, 0., 0., 238, 24
24, "CAM01", 1.0, "N", "52W034", 13.11264, 29.50106, 1950, 0., 0., 148, 25
25, "PHT22", 1.0, "N", "52W037", 13.11483, 29.63353, 1950, 0., 0., 657, 26
26, "PHT03", 1.0, "N", "52W037", 13.11483, 29.63353, 1950, 0., 0., 238, 27
27, "CAM01", 1.0, "N", "52W037", 13.11483, 29.63353, 1950, 0., 0., 148, 0
28, "PHT22", 1.0, "N", "53W005", 17.22288, 50.52856, 1950, 0., 0., 817, 29
29, "PHT03", 1.0, "N", "53W005", 17.22288, 50.52856, 1950, 0., 0., 238, 30
30, "CAM01", 1.0, "N", "53W005", 17.22288, 50.52856, 1950, 0., 0., 148, 31
31, "PHT22", 1.0, "N", "53W011", 17.23062, 49.98431, 1950, 0., 0., 657, 32
32, "PHT03", 1.0, "N", "53W011", 17.23062, 49.98431, 1950, 0., 0., 238, 33
33, "CAM01", 1.0, "N", "53W011", 17.23062, 49.98431, 1950, 0., 0., 148, 34
34, "PHT22", 1.0, "N", "53W025", 17.25219, 50.33647, 1950, 0., 0., 657, 35
35, "PHT03", 1.0, "N", "53W025", 17.25219, 50.33647, 1950, 0., 0., 238, 36
36, "CAM01", 1.0, "N", "53W025", 17.25219, 50.33647, 1950, 0., 0., 148, 37
37, "PHT22", 1.0, "N", "53W026", 17.25337, 49.84000, 1950, 0., 0., 657, 38
38, "PHT03", 1.0, "N", "53W026", 17.25337, 49.84000, 1950, 0., 0., 238, 39
39, "CAM01", 1.0, "N", "53W026", 17.25337, 49.84000, 1950, 0., 0., 148, 40
40, "PHT22", 1.0, "N", "53W027", 17.25337, 50.45189, 1950, 0., 0., 657, 41
41, "PHT03", 1.0, "N", "53W027", 17.25337, 50.45189, 1950, 0., 0., 238, 42
42, "CAM01", 1.0, "N", "53W027", 17.25337, 50.45189, 1950, 0., 0., 148, 43
43, "PHT22", 1.0, "N", "53W034", 17.26082, 50.06231, 1950, 0., 0., 657, 44
44, "PHT03", 1.0, "N", "53W034", 17.26082, 50.06231, 1950, 0., 0., 238, 45
45, "CAM01", 1.0, "N", "53W034", 17.26082, 50.06231, 1950, 0., 0., 148, 46
46, "PHT22", 1.0, "N", "53W035", 17.26140, 50.36378, 1950, 0., 0., 657, 47
47, "PHT03", 1.0, "N", "53W035", 17.26140, 50.36378, 1950, 0., 0., 238, 48
48, "CAM01", 1.0, "N", "53W035", 17.26140, 50.36378, 1950, 0., 0., 148, 0
49, "PHT22", 1.0, "N", "53W058", 17.30091, 50.01150, 1950, 0., 0., 817, 50
50, "PHT03", 1.0, "N", "53W058", 17.30091, 50.01150, 1950, 0., 0., 238, 51
51, "CAM01", 1.0, "N", "53W058", 17.30091, 50.01150, 1950, 0., 0., 148, 52
52, "PHT22", 1.0, "N", "53W062", 17.30462, 50.03478, 1950, 0., 0., 657, 53
53, "PHT03", 1.0, "N", "53W062", 17.30462, 50.03478, 1950, 0., 0., 238, 54
54, "CAM01", 1.0, "N", "53W062", 17.30462, 50.03478, 1950, 0., 0., 148, 55
55, "PHT22", 1.0, "N", "53W065", 17.30677, 50.01044, 1950, 0., 0., 657, 56
56, "PHT03", 1.0, "N", "53W065", 17.30677, 50.01044, 1950, 0., 0., 238, 57
57, "CAM01", 1.0, "N", "53W065", 17.30677, 50.01044, 1950, 0., 0., 148, 58
58, "PHT22", 1.0, "N", "53W068", 17.31202, 49.66722, 1950, 0., 0., 657, 59
59, "PHT03", 1.0, "N", "53W068", 17.31202, 49.66722, 1950, 0., 0., 238, 60
60, "CAM01", 1.0, "N", "53W068", 17.31202, 49.66722, 1950, 0., 0., 148, 61
61, "PHT22", 1.0, "N", "53W071", 17.31580, 50.33700, 1950, 0., 0., 657, 62
62, "PHT03", 1.0, "N", "53W071", 17.31580, 50.33700, 1950, 0., 0., 238, 63
63, "CAM01", 1.0, "N", "53W071", 17.31580, 50.33700, 1950, 0., 0., 148, 64
64, "PHT22", 1.0, "N", "53W072", 17.32091, 50.42569, 1950, 0., 0., 657, 65
65, "PHT03", 1.0, "N", "53W072", 17.32091, 50.42569, 1950, 0., 0., 238, 66
66, "CAM01", 1.0, "N", "53W072", 17.32091, 50.42569, 1950, 0., 0., 148, 67
67, "PHT22", 1.0, "N", "53W083", 17.34273, 50.09136, 1950, 0., 0., 657, 68
68, "PHT03", 1.0, "N", "53W083", 17.34273, 50.09136, 1950, 0., 0., 238, 69
69, "CAM01", 1.0, "N", "53W083", 17.34273, 50.09136, 1950, 0., 0., 148, 70
70, "PHT22", 1.0, "N", "53W090", 17.35241, 49.99175, 1950, 0., 0., 657, 71
71, "PHT03", 1.0, "N", "53W090", 17.35241, 49.99175, 1950, 0., 0., 238, 72
72, "CAM01", 1.0, "N", "53W090", 17.35241, 49.99175, 1950, 0., 0., 148, 0
73, "PHT22", 3.0, "N", "M003", 12.98487, 30.68556, 1950, 0., 0., 1841, 74
74, "CAM01", 3.0, "N", "M003", 12.98487, 30.68556, 1950, 0., 0., 182, 75
75, "PHT22", 3.0, "N", "M015", 12.99420, 30.72744, 1950, 0., 0., 1681, 76
76, "CAM01", 3.0, "N", "M015", 12.99420, 30.72744, 1950, 0., 0., 182, 77
77, "PHT22", 3.0, "N", "M022", 12.99648, 30.77558, 1950, 0., 0., 1681, 78
78, "CAM01", 3.0, "N", "M022", 12.99648, 30.77558, 1950, 0., 0., 182, 79
79, "PHT22", 3.0, "N", "M028", 12.99833, 30.71500, 1950, 0., 0., 1681, 80
80, "CAM01", 3.0, "N", "M028", 12.99833, 30.71500, 1950, 0., 0., 182, 81
81, "PHT22", 3.0, "N", "M043", 13.00347, 30.46131, 1950, 0., 0., 1681, 82
82, "CAM01", 3.0, "N", "M043", 13.00347, 30.46131, 1950, 0., 0., 182, 83
83, "PHT22", 3.0, "N", "M049", 13.00464, 30.57533, 1950, 0., 0., 1681, 84
84, "CAM01", 3.0, "N", "M049", 13.00464, 30.57533, 1950, 0., 0., 182, 0
85, "PHT22", 3.0, "N", "M051", 13.00489, 30.56292, 1950, 0., 0., 1841, 86
86, "CAM01", 3.0, "N", "M051", 13.00489, 30.56292, 1950, 0., 0., 182, 87
87, "PHT22", 3.0, "N", "M056", 13.00623, 30.79072, 1950, 0., 0., 1681, 88
88, "CAM01", 3.0, "N", "M056", 13.00623, 30.79072, 1950, 0., 0., 182, 89
89, "PHT22", 3.0, "N", "M063", 13.00770, 30.44881, 1950, 0., 0., 1681, 90
90, "CAM01", 3.0, "N", "M063", 13.00770, 30.44881, 1950, 0., 0., 182, 91
91, "PHT22", 3.0, "N", "M064", 13.00773, 30.57286, 1950, 0., 0., 1681, 92
92, "CAM01", 3.0, "N", "M064", 13.00773, 30.57286, 1950, 0., 0., 182, 93
93, "PHT22", 3.0, "N", "M097", 13.01548, 30.29394, 1950, 0., 0., 1681, 94
94, "CAM01", 3.0, "N", "M097", 13.01548, 30.29394, 1950, 0., 0., 182, 95
95, "PHT22", 3.0, "N", "M141", 13.03254, 30.60486, 1950, 0., 0., 1681, 96
96, "CAM01", 3.0, "N", "M141", 13.03254, 30.60486, 1950, 0., 0., 182, 0
<=== spring_launch_targets ===>
1, "PHT22", 2.0, "N", "52W005", 13.07429, 29.52150, 1950, 0., 0., 817, 2
2, "PHT03", 2.0, "N", "52W005", 13.07429, 29.52150, 1950, 0., 0., 238, 3
3, "CAM01", 2.0, "N", "52W005", 13.07429, 29.52150, 1950, 0., 0., 148, 4
4, "PHT22", 2.0, "N", "52W008", 13.08351, 29.30739, 1950, 0., 0., 657, 5
5, "PHT03", 2.0, "N", "52W008", 13.08351, 29.30739, 1950, 0., 0., 238, 6
6, "CAM01", 2.0, "N", "52W008", 13.08351, 29.30739, 1950, 0., 0., 148, 7
7, "PHT22", 2.0, "N", "52W012", 13.08995, 29.31747, 1950, 0., 0., 657, 8
8, "PHT03", 2.0, "N", "52W012", 13.08995, 29.31747, 1950, 0., 0., 238, 9
9, "CAM01", 2.0, "N", "52W012", 13.08995, 29.31747, 1950, 0., 0., 148, 10
10, "PHT22", 2.0, "N", "52W017", 13.09501, 29.59506, 1950, 0., 0., 657, 11
11, "PHT03", 2.0, "N", "52W017", 13.09501, 29.59506, 1950, 0., 0., 238, 12
12, "CAM01", 2.0, "N", "52W017", 13.09501, 29.59506, 1950, 0., 0., 148, 13
13, "PHT22", 2.0, "N", "52W020", 13.09931, 30.00050, 1950, 0., 0., 657, 14
14, "PHT03", 2.0, "N", "52W020", 13.09931, 30.00050, 1950, 0., 0., 238, 15
15, "CAM01", 2.0, "N", "52W020", 13.09931, 30.00050, 1950, 0., 0., 148, 16
16, "PHT22", 2.0, "N", "52W022", 13.10293, 29.83878, 1950, 0., 0., 657, 17
17, "PHT03", 2.0, "N", "52W022", 13.10293, 29.83878, 1950, 0., 0., 238, 18
18, "CAM01", 2.0, "N", "52W022", 13.10293, 29.83878, 1950, 0., 0., 148, 19
19, "PHT22", 2.0, "N", "52W023", 13.10321, 29.70731, 1950, 0., 0., 657, 20
20, "PHT03", 2.0, "N", "52W023", 13.10321, 29.70731, 1950, 0., 0., 238, 21
21, "CAM01", 2.0, "N", "52W023", 13.10321, 29.70731, 1950, 0., 0., 148, 22
22, "PHT22", 2.0, "N", "52W034", 13.11264, 29.50106, 1950, 0., 0., 657, 23
23, "PHT03", 2.0, "N", "52W034", 13.11264, 29.50106, 1950, 0., 0., 238, 24
24, "CAM01", 2.0, "N", "52W034", 13.11264, 29.50106, 1950, 0., 0., 148, 25
25, "PHT22", 2.0, "N", "52W037", 13.11483, 29.63353, 1950, 0., 0., 657, 26
26, "PHT03", 2.0, "N", "52W037", 13.11483, 29.63353, 1950, 0., 0., 238, 27
27, "CAM01", 2.0, "N", "52W037", 13.11483, 29.63353, 1950, 0., 0., 148, 0
28, "PHT22", 1.0, "N", "55W010", 8.54706, 45.12994, 1950, 0., 0., 817, 29
29, "PHT03", 1.0, "N", "55W010", 8.54706, 45.12994, 1950, 0., 0., 238, 30
30, "CAM01", 1.0, "N", "55W010", 8.54706, 45.12994, 1950, 0., 0., 148, 31
31, "PHT22", 1.0, "N", "55W020", 8.56172, 45.33967, 1950, 0., 0., 657, 32
32, "PHT03", 1.0, "N", "55W020", 8.56172, 45.33967, 1950, 0., 0., 238, 33
33, "CAM01", 1.0, "N", "55W020", 8.56172, 45.33967, 1950, 0., 0., 148, 34
34, "PHT22", 1.0, "N", "55W027", 8.56549, 45.15025, 1950, 0., 0., 657, 35
35, "PHT03", 1.0, "N", "55W027", 8.56549, 45.15025, 1950, 0., 0., 238, 36
36, "CAM01", 1.0, "N", "55W027", 8.56549, 45.15025, 1950, 0., 0., 148, 37
37, "PHT22", 1.0, "N", "55W034", 8.56917, 45.59744, 1950, 0., 0., 657, 38
38, "PHT03", 1.0, "N", "55W034", 8.56917, 45.59744, 1950, 0., 0., 238, 39
39, "CAM01", 1.0, "N", "55W034", 8.56917, 45.59744, 1950, 0., 0., 148, 40
40, "PHT22", 1.0, "N", "55W036", 8.57099, 45.26286, 1950, 0., 0., 657, 41
41, "PHT03", 1.0, "N", "55W036", 8.57099, 45.26286, 1950, 0., 0., 238, 42
42, "CAM01", 1.0, "N", "55W036", 8.57099, 45.26286, 1950, 0., 0., 148, 43
43, "PHT22", 1.0, "N", "55W049", 8.59330, 44.84789, 1950, 0., 0., 657, 44
44, "PHT03", 1.0, "N", "55W049", 8.59330, 44.84789, 1950, 0., 0., 238, 45
45, "CAM01", 1.0, "N", "55W049", 8.59330, 44.84789, 1950, 0., 0., 148, 46
46, "PHT22", 1.0, "N", "55W066", 8.61446, 45.27142, 1950, 0., 0., 657, 47
47, "PHT03", 1.0, "N", "55W066", 8.61446, 45.27142, 1950, 0., 0., 238, 48
48, "CAM01", 1.0, "N", "55W066", 8.61446, 45.27142, 1950, 0., 0., 148, 49
49, "PHT22", 1.0, "N", "55W077", 8.62513, 44.75519, 1950, 0., 0., 657, 50
50, "PHT03", 1.0, "N", "55W077", 8.62513, 44.75519, 1950, 0., 0., 238, 51
51, "CAM01", 1.0, "N", "55W077", 8.62513, 44.75519, 1950, 0., 0., 148, 52
52, "PHT22", 1.0, "N", "55W097", 8.64174, 44.89975, 1950, 0., 0., 657, 53
53, "PHT03", 1.0, "N", "55W097", 8.64174, 44.89975, 1950, 0., 0., 238, 54
54, "CAM01", 1.0, "N", "55W097", 8.64174, 44.89975, 1950, 0., 0., 148, 55
55, "PHT22", 1.0, "N", "55W102", 8.64635, 45.08136, 1950, 0., 0., 657, 56
56, "PHT03", 1.0, "N", "55W102", 8.64635, 45.08136, 1950, 0., 0., 238, 57
57, "CAM01", 1.0, "N", "55W102", 8.64635, 45.08136, 1950, 0., 0., 148, 58
58, "PHT22", 1.0, "N", "55W135", 8.68826, 44.54200, 1950, 0., 0., 657, 59
59, "PHT03", 1.0, "N", "55W135", 8.68826, 44.54200, 1950, 0., 0., 238, 60
60, "CAM01", 1.0, "N", "55W135", 8.68826, 44.54200, 1950, 0., 0., 148, 61
61, "PHT22", 1.0, "N", "55W137", 8.68968, 44.92561, 1950, 0., 0., 657, 62
62, "PHT03", 1.0, "N", "55W137", 8.68968, 44.92561, 1950, 0., 0., 238, 63
63, "CAM01", 1.0, "N", "55W137", 8.68968, 44.92561, 1950, 0., 0., 148, 0
64, "PHT22", 1.0, "N", "55W144", 8.69831, 45.20311, 1950, 0., 0., 817, 65
65, "PHT03", 1.0, "N", "55W144", 8.69831, 45.20311, 1950, 0., 0., 238, 66
66, "CAM01", 1.0, "N", "55W144", 8.69831, 45.20311, 1950, 0., 0., 148, 67
67, "PHT22", 1.0, "N", "55W150", 8.70149, 45.02614, 1950, 0., 0., 657, 68
68, "PHT03", 1.0, "N", "55W150", 8.70149, 45.02614, 1950, 0., 0., 238, 69
69, "CAM01", 1.0, "N", "55W150", 8.70149, 45.02614, 1950, 0., 0., 148, 70
70, "PHT22", 1.0, "N", "55W153", 8.70231, 45.11897, 1950, 0., 0., 657, 71
71, "PHT03", 1.0, "N", "55W153", 8.70231, 45.11897, 1950, 0., 0., 238, 72
72, "CAM01", 1.0, "N", "55W153", 8.70231, 45.11897, 1950, 0., 0., 148, 73
73, "PHT22", 1.0, "N", "55W158", 8.71144, 44.69794, 1950, 0., 0., 657, 74
74, "PHT03", 1.0, "N", "55W158", 8.71144, 44.69794, 1950, 0., 0., 238, 75
75, "CAM01", 1.0, "N", "55W158", 8.71144, 44.69794, 1950, 0., 0., 148, 76
76, "PHT22", 1.0, "N", "55W171", 8.72870, 44.56303, 1950, 0., 0., 657, 77
77, "PHT03", 1.0, "N", "55W171", 8.72870, 44.56303, 1950, 0., 0., 238, 78
78, "CAM01", 1.0, "N", "55W171", 8.72870, 44.56303, 1950, 0., 0., 148, 79
79, "PHT22", 1.0, "N", "55W175", 8.73627, 44.25367, 1950, 0., 0., 657, 80
80, "PHT03", 1.0, "N", "55W175", 8.73627, 44.25367, 1950, 0., 0., 238, 81
81, "CAM01", 1.0, "N", "55W175", 8.73627, 44.25367, 1950, 0., 0., 148, 82
82, "PHT22", 1.0, "N", "55W178", 8.73918, 44.76461, 1950, 0., 0., 657, 83
83, "PHT03", 1.0, "N", "55W178", 8.73918, 44.76461, 1950, 0., 0., 238, 84
84, "CAM01", 1.0, "N", "55W178", 8.73918, 44.76461, 1950, 0., 0., 148, 85
85, "PHT22", 1.0, "N", "55W183", 8.74381, 44.73611, 1950, 0., 0., 657, 86
86, "PHT03", 1.0, "N", "55W183", 8.74381, 44.73611, 1950, 0., 0., 238, 87
87, "CAM01", 1.0, "N", "55W183", 8.74381, 44.73611, 1950, 0., 0., 148, 88
88, "PHT22", 1.0, "N", "55W184", 8.74430, 44.65972, 1950, 0., 0., 657, 89
89, "PHT03", 1.0, "N", "55W184", 8.74430, 44.65972, 1950, 0., 0., 238, 90
90, "CAM01", 1.0, "N", "55W184", 8.74430, 44.65972, 1950, 0., 0., 148, 91
91, "PHT22", 1.0, "N", "55W188", 8.75083, 44.87644, 1950, 0., 0., 657, 92
92, "PHT03", 1.0, "N", "55W188", 8.75083, 44.87644, 1950, 0., 0., 238, 93
93, "CAM01", 1.0, "N", "55W188", 8.75083, 44.87644, 1950, 0., 0., 148, 94
94, "PHT22", 1.0, "N", "55W191", 8.75454, 44.21789, 1950, 0., 0., 657, 95
95, "PHT03", 1.0, "N", "55W191", 8.75454, 44.21789, 1950, 0., 0., 238, 96
96, "CAM01", 1.0, "N", "55W191", 8.75454, 44.21789, 1950, 0., 0., 148, 97
97, "PHT22", 1.0, "N", "55W199", 8.76192, 44.54136, 1950, 0., 0., 657, 98
98, "PHT03", 1.0, "N", "55W199", 8.76192, 44.54136, 1950, 0., 0., 238, 99
99, "CAM01", 1.0, "N", "55W199", 8.76192, 44.54136, 1950, 0., 0., 148, 0