6603( 3) - 02/16/96 17:50 - [ 1]
PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only
ID: 6603
Version: 3
Check-in Date: 16-Feb-1996
17:44:29
1.Proposal Title:
Probing Proto-Planetary Disks in the Orion Nebula
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2. Scientific Category 3. Proposal For 4. Cycle
BINARIES AND STAR FOR GO 6
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5. Investigators
Contact?
PI: John Bally University of Colorado
CoI: Mark McCaughrean Max Planck Institute for Astronomy, N
Heidelberg
CoI: C. Robert O'Dell Rice University N
CoI: Ralph Sutherland Mt. Stromolo and Siding Spring N
Observatories
CoI: David Devine University of Colorado N
6603( 3) - 02/16/96 17:50 - [ 2]
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6. Abstract
We will probe fundamental physical properties and structures of recently discovered,
and uniquely visible, protoplanetary disks around young stars in the Orion Nebula
(M42, NGC1976). We will obtain narrow band and continuum images with the maximum
possible angular resolution and use orders of magnitude deeper integrations than
previously attempted. We will achieve images of protoplanetary disks with a linear
resolutions of ~ 5 to 20 A.U., a factor a 2 to 5 improvement over previous HST
results. It is vital to carry out these new high resolution deep integrations
because accurate determinations of absorption profiles will be fundamental in
constraining models of disks and their interactions with the nebula environment.
There is also the exciting possibility of detecting absorption profile ``gaps'' or
rings on A.U. scales that could be direct evidence for extra--solar planets. Hence,
our primary objectives are to obtain: 1 Deep PC & WFC images of a small number of
selected objects (discovered in Cycle 4 & 5) which we believe to be disks seen in
silhouette, or are disks in ionized envelopes, 2 Deep UV images with the FOC of pure
dark objects that lie in front of the brightest portion of the Orion Nebula. 3
Proper motion determinations of fast compact nebular components. Using earlier epoch
HST data, our Cycle 6 WFPC2 images will give a proper motion sensitivity (> 40 Delta
t_years^-1 kms) allowing us to detect moving gas from stationary nebula gas.
Observing_Description Description of Primary Targets NGC1976-HST16 This is the
largest dark disk that is seen relatively face on. We will take very deep images in
three narrow-band filters with the PC in an attempt to obtain an accurate radial
profile for the dust distribution and its wavelength dependence, and to look for
gaps that may indicate giant planet formation. We plan to integrate a full orbit in
the FOC F220W filter in an attempt to obtain 8 AU angular resolution which can be
used to set limits on gaps as narrow as a fraction of an AU under the back lit
circumstances of HST 16. NGC1976-HST10 field HST 10 is a tear drop shaped bright
proplyd that contains a 1' diameter edge-on disk. Its central star is not visible
out to Lambda = 3.8Mum. It is either a flattened starless core or an edge-on
circumstellar disk with at least 50 to 100 magnitudes of visual extinction. This
object exhibits the strongest H_2 S(1) line of any of the proplyds observed at the
IRTF. UV observations for a full orbit will be used to compare the disk properties
at UV and red wavelengths, obtain constraints on grain properties, and to look for
pile of up of dust near the ionization front. HST 10 will fall in the same PC frame
as HST16, so it will be be reobserved with a factor of two better resolution and 10
times longer integration than previous (Cycle 4 & 5) data, with no additional
integrations. NGC1976-SW It is a 2"\\ diameter silhouetted disk seen edge on that
contains an obscured star whose radiation illuminates cones of visual and near--IR
light along its minor axis. The star has not been detected directly even at 1
micron, implying a large line--of--sight extinction. We plan two orbits for
polarimetry with broad-band WFC filters (POLQ + F606W). In these filters, the
reflection cones will be relatively bright (providing a signal of about 3
electron/second in a PC pixel. The reflection cone is expected to be highly
polarized. The polarization data will constrain the source geometry as well as the
dust properties. We plan obtain dithered PC observations of this object in 2 narrow
band filters, (chosen to contain the brightest background fluxes) in an attempt to
obtain the radial and vertical column density profiles. We will also obtain a full
orbit integration in a far red broad- band filter in order to detect the central
star, or obtain a lower limit in the opacity towards it. This will also allow us to
determine a lower limit to the total dust mass in the disk, a vital parameter. In
each orbit, we will use sub-pixel sub-stepping to reach the full angular resolution
of HST. The discovery observations of SW are qualitatively consistent with edge-on
embedded YSOs modeled by Whitney & Hartmann (1992, ApJ, 395, 529; 1993, ApJ, 402,
605), and we expect that the more quantitative comparisons that will be possible
with the new data will help us determine the vertical structure in the disk and the
diffuse scattering halo surrounding it. NGC1976-HST8 This is one of the largest
cometary teardrop shaped proplyds in the Orion Nebula. It contains both a visible
star and a dark disk inside the ionized teardrop. It is illuminated by Theta ^2A
Ori, an O9 star below the Orion Bar. This object was discovered in the pre-repair
mission images O'Dell, Wen, and Hu (1993). Full orbit sub-stepped images in narrow
band filters will characterize the disk and ionization conditions. NGC1976-PC151,
NGC1976-WF1, NGC1976-PC10, NGC1976-SIX, NGC1976-SEVEN These are all dark silhouette
proplyds discovered during the Cycle 4 & 5 surveys. Most are small (sub- arcsecond),
and the present WFC images are poorly resolved. Therefore we will obtain PC images
in a single bright emission line (HAlpha, F656N), using sub-pixel dithering to
obtain the full resolution at that wavelength. Each disk will be given one orbit.
These observations will define the radial extent and other characteristics of of
these disks, and in combination with the other dark disk observations, will provide
us with the first opportunity to determine the statistical properties of set of YSO
disks. NGC1976-LV5 This single FOC pointing contains 5 proplyds. These objects lie
very close to the Trapezium and are the brightest of the cometary proplyds (similar
to the ones shown in Figure 1 frames 1, 2, and 4). Our Cycle 4 short exposures show
tantalizing evidence of dark disks inside the bright cometary shapes. Full orbit
wide band images will delineate these disks clearly. Data will be used for analysis
of proplyd morphology and its relation to the central star properties (mostly
determined from near-IR and ground based visual spectra) and location within the M42
core. FOC images will use spectral elements that include the brightest UV emission
features. Exposure times for the above sources are based on our ERO and Cycle 4
data, scaled to PC (or FOC) resolution, with the requirement that at least 2 high
S/N exposures are needed in each dithered position for cosmic ray rejection.
Parallel Observations We will use WFPC2 to obtain narrow band parallel observations
while we perform primary data acquisition on the FOC. This data will permit coverage
of outlying regions of M42 not covered by primary WFPC2 targeting and will greatly
increase the area of the sky in which proplyds, shock excited nebulae (Herbig-Haro)
objects and stellar jets, have been searched. The roll requirements for HST will be
determined by the desire to make WFPC2 coverage of the Orion Nebula complete as
possible. This should allow completion of coverage of M43, a nearby and simpler HII
region which is partially covered by Cycle 4 parallel observations. Related
Observations Optical We have used facilities at Kitt Peak National Observatory, the
ESO New Technology Telescope, and the facilities at McDonald Observatory to obtain
high dispersion spectra of the proplyds and the surrounding nebula (Coude feed and
McDonald Cas spectrometer), and to acquire narrow band images of the nebula with the
best angular resolution possible from the ground (with the NTT). Near Infrared Near
infrared observations of the 2.1218Mum S(1) line of H_2 obtained in November 1994
with the IRTF (with CSHELL) resulted in the detection of strong H_2 emission
(considerably brighter than that produced by the background molecular cloud) from 8
out of 10 proplyds, including HST 1 and HST 10. This data demonstrates the existence
of large quantities of molecular gas between the proplyd ionization front and the
central star. The H_2 emission is likely to be excited by incident UV light.
Although HST 10 has the brightest H_2 emission of any proplyd studied so far, the
dark object HST 16 was not detected, probably due to insufficient UV excitation.
McCaughrean, Zinnecker, Rayner, and Stauffer have obtained 1 to 4micron (JHKL)
imaging photometry of the Trapezium Cluster on Calar Alto and at the IRTF\\@. These
data will be combined with existing and new HST V and I imaging photometry, as well
as optical spectroscopy, in order to determine the ages and masses of the cluster
stars. These stellar parameters will be used in the analysis of the proplyds, as
they play a role in the disk structure and dynamics. Also, they help constrain the
inner edge of the disk, as the majority of all Trapezium stars are found to show
excess 4micron flux, thought to arise in that region (McCaughrean et al. 1994:
http://spitfire.mpia- hd.mpg.de/Preprints.html ``Circumstellar disks in the
Trapezium Cluster''). Millimeter Wavelengths We have applied for time to use the
Owens Valley Interferometer to search for millimeter-wavelength emission from the
proplyds, in order to determine the total dust mass from the continuum emission, and
the cold gas mass and dynamics traced by the J=2--1 isotopes of CO\\@. From the mm-
wave continuum, we can estimate the total dust mass present. Although optical
obscuration is not a reliable dust indicator for the proplyds, a comparison of the
optical extinction and millimeter dust emission can provide constraints of the grain
sizes. The width of mm-wavelength spectral lines will provide kinematic constraints
on the mass of the central star, since for the largest proplyds, we may detect
Keplerian rotation. From the integrated line flux, we can estimate the total column
density of the molecules, and combine this with the continuum to estimate gas to
dust ratios, depletions, and hopefully the total mass of the protoplanetary disks.
Other These observations provide us with the best available optical and ground based
data on these objects. This data, together with the ionization code, MAPPINGS II
(Sutherland & Dopita 1992, ApJS, 88, 253) are being used to analyze spectral lines
extending from the UV to the near-IR data to infer ionization and excitation
conditions in and around the proplyds. Detailed theoretical dust models which can
take into account classical grains and small organic grains in various mixtures will
be used to model the dust front physics.
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6603( 3) - 02/16/96 17:50 - [ 3]
Data Distribution
Media: 8MM
Blocking Factor: 10
Ship To: *John Bally*CASA, Campus Box
389*University of Colorado*Boulder, CO
80309
Ship Via: UPS
Email: ,
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6603( 3) - 02/16/96 17:50 - [ 4]
TARGET LIST a) Fixed Targets
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Tar| Target | Target | Target |Coord | Radial | Flux data
No | Name | Description | Position |Eqnx | Vel. |
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1 NGC1976- ISM, HII REGION,STAR,T RA=05H 35M 18.26S +/- 1.0",DEC=- 2000 F-LINE(6563)=5+/-1e-13
HST10-16 TAURI STAR 05D 24' 09.2" +/- 1.0"
Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec)
2000 0.0 0.0 0.0
2 NGC1976-SW ISM, HII REGION,STAR,T RA=05H 35M 11.35S +/- 1.0",DEC=- J2000 F-LINE(6563)=-5+/-1e-13
TAURI STAR 05D 24' 26.3" +/- 1.0"
Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec)
J2000 0.0 0.0 0.0
3 NGC1976- ISM, HII REGION,STAR,T RA=05H 35M 16.63S +/- 1.0",DEC=- 2000 F-LINE(6563)=5+/-1e-13
PC151-SIX TAURI STAR 05D 22' 42.6" +/- 1.0"
Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec)
2000 0.0 0.0 0.0
4 NGC1976-WF1 ISM, HII REGION,STAR,T RA=05H 35M 21.80S +/- 1.0",DEC=- 2000 F-LINE(6563)=5+/-1e-13
TAURI STAR 05D 23' 54.06" +/- 1.0"
Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec)
2000 0.0 0.0 0.0
5 NGC1976- ISM, HII REGION,STAR,T RA=05H 35M 15.83S +/- 1.0",DEC=- 2000 F-LINE(6563)=5+/-1e-13
LV6VLA10 TAURI STAR 05D 23' 25.65" +/- 1.0"
Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec)
2000 0.0 0.0 0.0
6 NGC1976- ISM, HII REGION,STAR,T RA=05H 35M 18.32S +/- 1.0",DEC=- 2000 F-LINE(6563)=-5+/-1e-13
HST16 TAURI STAR 05D 24' 05.0" +/- 1.0"
Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec)
2000 0.0 0.0 0.0
7 NGC1976-HST1 ISM, HII REGION,STAR,T RA=05H 35M 17.67S +/- 1.0",DEC=- 2000 F-LINE(6563)=5+/-1e-13
TAURI STAR 05D 23' 41.0" +/- 1.0"
Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec)
2000 0.0 0.0 0.0
8 NGC1976-HST8 ISM, HII REGION,STAR,T RA=05H 35M 20.14S +/- 1.0",DEC=- 2000 F-LINE(6563)=5+/-1e-13
-9 TAURI STAR 05D 24' 36.66" +/- 1.0"
Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec)
2000 0.0 0.0 0.0
9 NGC1976-PC10 ISM, HII REGION,STAR,T RA=05H 35M 12.10S +/- 1.0",DEC=- 2000 F-LINE(6563)=5+/-1e-13
TAURI STAR 05D 19' 25.1" +/- 1.0"
Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec)
2000 0.0 0.0 0.0
10 NGC1976- ISM, HII REGION,STAR,T RA=05H 35M 18.21S +/- 1.0",DEC=- 2000 F-LINE(6563)=5+/-1e-13
HST10 TAURI STAR 05D 24' 13.3" +/- 1.0"
Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec)
2000 0.0 0.0 0.0
6603( 3) - 02/16/96 17:50 - [ 5]
Visit: 01
Visit Requirements: ORIENT 310D TO 320D
On Hold Comments: <none>
Additional Comments: U3PA=315+/-5
Exposures
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Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special
Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements
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1 NGC1976- WFPC2 IMAGE PC1 F502N 5007 DITHER-TYPE=BOX 1 400S
HST10-16
Comments: [OIII]
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2 NGC1976- WFPC2 IMAGE PC1 F658N 6584 DITHER-TYPE=BOX 1 400S
HST10-16
Comments: [NII]
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3 NGC1976- WFPC2 IMAGE PC1 F658N 6584 1 60S
HST10-16
Comments: [NII]
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4 NGC1976- WFPC2 IMAGE PC1 F656N 6563 DITHER-TYPE=BOX 1 400S
HST10-16
Comments: Ha
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5 NGC1976- WFPC2 IMAGE PC1 F656N 6563 1 60S
HST10-16
Comments: Ha
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6603( 3) - 02/16/96 17:50 - [ 6]
Visit: 02
Visit Requirements: ORIENT 65D TO 75D
On Hold Comments: <none>
Additional Comments: U3PA=70D+/-5
Exposures
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Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special
Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements
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6 NGC1976-SW WFPC2 IMAGE PC1 F502N 5007 DITHER-TYPE=BOX 1 400S
Comments: [OIII]
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7 NGC1976-SW WFPC2 IMAGE PC1 F656N 6563 DITHER-TYPE=BOX 1 400S
Comments: Ha
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8 NGC1976-SW WFPC2 IMAGE PC1 F656N 6563 1 60S
Comments: Short Ha
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9 NGC1976-SW WFPC2 IMAGE PC1 F814W DITHER-TYPE=BOX 1 400S
Comments: CONTINUUM
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10 NGC1976-SW WFPC2 IMAGE PC1 F814W 1 60S
Comments: SHORT CONTINUUM
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11 NGC1976-SW WFPC2 IMAGE PC1 F606W,POL DITHER- 1 300S
Q TYPE=LINE
Comments: POLARIZATION PA=135D
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12 NGC1976-SW WFPC2 IMAGE WF2 F606W,POL DITHER- 1 300S
Q TYPE=LINE
Comments: POLARIZATION PA=0D
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13 NGC1976-SW WFPC2 IMAGE WF3 F606W,POL DITHER- 1 300S
Q TYPE=LINE
Comments: POLARIZATION PA=45D
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14 NGC1976-SW WFPC2 IMAGE WF4 F606W,POL DITHER- 1 300S
Q TYPE=LINE
Comments: POLARIZATION PA=90D
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6603( 3) - 02/16/96 17:50 - [ 7]
Visit: 03
Visit Requirements: ORIENT 95D TO 105D
On Hold Comments: <none>
Additional Comments: U3PA=100D+/-5
Exposures
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Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special
Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements
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15 NGC1976- WFPC2 IMAGE PC1 F656N 6563 DITHER-TYPE=BOX 2 160S
PC151-SIX
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16 NGC1976- WFPC2 IMAGE PC1 F656N 6563 1 200S
PC151-SIX
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17 NGC1976- WFPC2 IMAGE PC1 F656N 6563 DITHER-TYPE=BOX 2 160S
HST1
Comments: SEVEN. COPY OF CYCLE 4 POINTING
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18 NGC1976- WFPC2 IMAGE PC1 F656N 6563 1 200S
HST1
Comments: SEVEN. COPY OF CYCLE 4 POINTING
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19 NGC1976- WFPC2 IMAGE PC1 F656N 6563 DITHER-TYPE=BOX 1 400S
PC10
Comments: EXTEND MOSAIC TO N
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6603( 3) - 02/16/96 17:50 - [ 8]
Visit: 04
Visit Requirements: ORIENT 250D TO 260D
On Hold Comments: <none>
Additional Comments: U3PA=255D+/-5
Exposures
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Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special
Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements
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20 NGC1976-WF1 WFPC2 IMAGE PC1 F656N 6563 DITHER-TYPE=BOX 1 400S
Comments: EXTEND WF MOSAIC TO EAST
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21 NGC1976- WFPC2 IMAGE PC1 F502N 5007 DITHER-TYPE=BOX 1 400S
HST8-9
Comments: [OIII], WF COVERS HH203 AND HH204
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22 NGC1976- WFPC2 IMAGE PC1 F502N 5007 1 60S
HST8-9
Comments: SHORT [OIII], WF COVERS HH203 AND HH204
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23 NGC1976- WFPC2 IMAGE PC1 F631N 6300 DITHER-TYPE=BOX 1 400S
HST8-9
Comments: [OI], WF COVERS HH203 AND HH204
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24 NGC1976- WFPC2 IMAGE PC1 F631N 6300 1 60S
HST8-9
Comments: SHORT [OI], WF COVERS HH203 AND HH204
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25 NGC1976- WFPC2 IMAGE PC1 F656N 6563 DITHER-TYPE=BOX 1 400S
HST8-9
Comments: HA, WF COVERS HH203 AND HH204
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26 NGC1976- WFPC2 IMAGE PC1 F656N 6563 1 60S
HST8-9
Comments: SHORT HA, WF COVERS HH203 AND HH204
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27 NGC1976- WFPC2 IMAGE PC1 F658N 6583 DITHER-TYPE=BOX 1 400S
HST8-9
Comments: [NII], WF COVERS HH203 AND HH204
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28 NGC1976- WFPC2 IMAGE PC1 F658N 6583 1 60S
HST8-9
Comments: SHORT [NII], WF COVERS HH203 AND HH204
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6603( 3) - 02/16/96 17:50 - [ 9]
Visit: 05
Visit Requirements: ORIENT 265D TO 275D
On Hold Comments: <none>
Additional Comments: U3PA=270D+/-5
Exposures
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Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special
Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements
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29 NGC1976- FOC/96 IMAGE 512X512 F220W 2200 1 1100S
HST16
Comments: UV CONTINUUM
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30 NGC1976- WFPC2 IMAGE PC1 F656N 6563 1 900S PAR WITH 29
HST16
Comments: WF EXTENDS Ha MOSAIC NW
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31 NGC1976- FOC/96 IMAGE 512X512 F220W 2200 1 1100S POS TARG +0.3535, +0.3535
HST16
Comments: UV CONTINUUM
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32 NGC1976- WFPC2 IMAGE PC1 F656N 6563 1 900S PAR WITH 31
HST16
Comments: WF EXTENDS Ha MOSAIC NW
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33 NGC1976- FOC/96 IMAGE 512X512 F220W 2200 1 1100S
HST10
Comments: UV CONTINUUM
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34 NGC1976- WFPC2 IMAGE PC1 F673N 6731 1 900S PAR WITH 33
HST10
Comments: WF EXTENDS [SII] MOSAIC NW
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35 NGC1976- FOC/96 IMAGE 512X512 F220W 2200 1 1100S POS TARG +0.3535, +0.3535
HST10
Comments: UV CONTINUUM
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36 NGC1976- WFPC2 IMAGE PC1 F673N 6731 1 900S PAR WITH 35
HST10
Comments: WF EXTENDS [SII] MOSAIC NW
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37 NGC1976- FOC/96 IMAGE 512X512 F220W 2200 1 1100S
LV6VLA10
Comments: UV CONTINUUM
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38 NGC1976- WFPC2 IMAGE PC1 F658N 6584 1 900S PAR WITH 37
LV6VLA10
Comments: WF EXTENDS [NII] MOSAIC NW
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39 NGC1976- FOC/96 IMAGE 512X512 F220W 2200 1 1100S POS TARG +0.3535, +0.3535
LV6VLA10
Comments: UV CONTINUUM
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6603( 3) - 02/16/96 17:50 - [ 10]
Exposures
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Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special
Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements
------------------------------------------------------------------------------------------------------------------------------------
40 NGC1976- WFPC2 IMAGE PC1 F658N 6584 1 900S PAR WITH 39
LV6VLA10
Comments: WF EXTENDS [NII] MOSAIC NW
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41 NGC1976- FOC/96 IMAGE 512X512 F220W 2200 1 1100S
HST1
Comments: UV CONTINUUM
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42 NGC1976- WFPC2 IMAGE PC1 F502N 5007 1 900S PAR WITH 41
HST1
Comments: WF EXTENDS [OIII] MOSAIC NW
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43 NGC1976- FOC/96 IMAGE 512X512 F220W 2200 1 1100S POS TARG +0.3535, +0.3535
HST1
Comments: UV CONTINUUM
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44 NGC1976- WFPC2 IMAGE PC1 F502N 5007 1 900S PAR WITH 43
HST1
Comments: WF EXTENDS [OIII] MOSAIC NW
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6603( 3) - 02/16/96 17:50 - [ 11]
Summary Form for Proposal 6603
Item Used in this proposal
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Configurations WFPC2 FOC/96
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Opmodes IMAGE
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Optional Parameters DITHER-TYPE=BOX DITHER-TYPE=LINE
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Proposal Category GO
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Scientific Category BINARIES AND STAR FORMATION
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Special Requirements ORIENT 310D TO 320D ORIENT 65D TO 75D ORIENT 95D TO 105D ORIENT 250D TO 260D ORIENT 265D TO 275D
PAR WITH 29 POS TARG +0.3535, +0.3535 PAR WITH 31 PAR WITH 33 PAR WITH 35 PAR WITH 37 PAR WITH 39
PAR WITH 41 PAR WITH 43
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Spectral Elements F502N F658N F656N F814W F606W,POLQ F631N F220W F673N
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Target Names NGC1976-HST10-16 NGC1976-SW NGC1976-PC151-SIX NGC1976-HST1 NGC1976-PC10 NGC1976-WF1 NGC1976-HST8-9
NGC1976-HST16 NGC1976-HST10 NGC1976-LV6VLA10
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