0Assigned ID: 7081
----- Attempting Submission 1 (Tue Apr 14 17:48:42 GMT 2026) -----
HST Phase I Proposal 7081 successfully submitted.
Receipt: # 7081-1
----- Attempting Submission 2 (Tue Apr 14 18:18:40 GMT 2026) -----
HST Phase I Proposal 7081 successfully submitted.
Receipt: # 7081-2
----- Attempting Submission 3 (Tue Apr 14 20:37:16 GMT 2026) -----0----- Attempting Submission 1 (Sun Aug 16 11:57:34 GMT 2026) -----The target tool has been run but the APT hangs when it runs so I have to restart the APT.The First Direct Measurement of UV Extinction Curves Outside the Local Group in the LMC-like galaxy, NGC 55The observations proposed here will be the first UV spectra of reddened OB stars in the Sculptor galaxy, NGC 55, using HST/STIS. These new observations will be used to make the first direct measurements of UV extinction properties in a galaxy outside the Local Group. The UV extinction properties of interstellar dust have now been surveyed for five galaxies in the Local Group (MW, LMC, SMC, M31, M33). There is a family of UV extinction curves that describes the Local Group. Is this family of extinction curves present in other more distant galaxies or is it unique to the Local Group? It is necessary to study a galaxy, outside the Local Group yet close enough for individual stars to be observed. NGC 55 bears a very close resemblance to the LMC in both morphology and metallicity. This makes it likely that the new observations will show significant variations in the dust extinction properties across NGC 55. Extinction curves will be constructed using the standard pair method where observations of the reddened star are compared to a stellar atmosphere model of the same spectral type. In order to analyze the composition and size distributions of the dust grain population,s Maximum Entropy Modeling will be used. The results will be used to provide more accurate dust parameters for radiative transfer modeling of galaxies which cannot be done without a detailed knowledge of the characteristics of this absorbing medium. We are proposing to observe five stars in NGC 55 using HST/STIS and the G140L, G230L, and G430L gratings that will sample the dust in the 30-Dor-like regions in NGC 55 as well as in other parts of the galaxy.The small aperture and high sensitivity of HST/STIS are ideal for obtaining UV spectra of
stars in the crowded fields of NGC 55. The ability to use the 0.2 x 0.2 slit will allow us
to avoid including close neighbors. HST imaging has been examined for each of the targets
to confirm that they are single stars (Dalcanton et al., 2009). The entire wavelength range
covered by the G140L (1150-1730 A) and G230L (1570-3180 A) gratings is needed to obtain the UV extinction curve, including the near-UV, the 2175A bump, and the far-UV rise.
In addition, the stars will be observed with the G430L grating. The wavelengths sampled
with the G430L grating spectroscopy will furnish critical temperature and surface gravity
diagnostics that are essential to disentangle the slope of the UV extinction from stellar effects.
In particular, measuring the size of the Balmer Jump (3645 A) aids in choosing the closest
atmosphere model for comparison.
Using the STIS ETC and assuming a B0I star with V=20.0, and reddening of E(B-V) =
0.3, the exposures in both UV gratings can be obtained in three orbits each with an average
S/N >10 if one bins 7 pixels. A similar S/N of >10 can be obtained for the G430L grating
in one orbit. These calculations assume Cardelli et al. (1989) R(V)= 3.1 extinction. If the
extinction is more LMC/SMC-like, one can bin more pixels to get the required S/N. Good
S/N UV spectra using HST/STIS have been obtained in one orbit using the G140L and
G230L gratings for stars in M31 and M33 with similar reddenings and spectral types as the
proposed targets in NGC 55 (Clayton et al., 2025; Gordon et al., 2026). The NGC 55 stars
are about one magnitude fainter on average, so three orbits per target are required for the
UV gratings. The targets are all between early-B and mid-O type and have V magnitudes
=19th, well below the bright limits for the MAMAs.
NGC 55 has orbit visibilities of about 51 minutes. The first orbit for each target has an
overhead of 17.5 minutes including GS Acq, STIS/ACQ, and grating overhead. The second
to fourth orbits have overheads of 11.5-14.5 minutes including the GS Reacq and the grating
overhead. The G430L grating will be done during the first orbit for each target. So, the
G430L grating will have an exposure of 2010s, and the G140L and G230L will have total
exposures from the three orbits of 6930s. Since the observations are using the 0.2 x 0.2 slit
no peakup is required. The plan is to observe a total of 5 stars in NGC 55 for 7 orbits per
star. Therefore, 35 orbits are requested.The PI, Geoff Clayton, and Co-I, Karl Gordon, are long-term experts in measuring, analyzing, and modeling dust extinction at UV, optical, and IR wavelengths. They also have a significant amount of experience in using HST/STIS spectra for extinction measurements.
Marjorie Decleir, is an expert in interstellar dust studies both in the Milky Way and in nearby galaxies. Her experience with measuring extinction curves based on stellar models will greatly benefit this work.
Petia Yanchulova Merica-Jones has expertise in studying dust extinction properties in the Magellanic Clouds and other Local Group galaxies using HST/STIS spectra.
Ralph Bohlin is a world expert in space instrument calibration. He has worked as a calibration scientist at STSCI for most of his career and calibrated the STIS instrument.Stellar Populations and the Interstellar MediumGalaxies6falsetruefalsefalsefalsefalsefalseSUPPORTEDEXT-STARB0-B2 III-INOJ2000J2000V-I=0.03EXT-STARB0-B2 III-IJ2000J2000V-I=0.045EXT-STARB0-B2 III-IJ2000J2000V-I=0.56EXT-STARB0-B2 III-IJ2000J2000V-I=0.14EXT-STARSUPERGIANT OJ2000J2000V-I=0.10STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/CCDSpectroscopicNoNoG430L4300/private/var/folders/_v/tncnbm8s77q2cv5jlfjlpw580000gn/T/OPVisit4277815898161762578.xmlThe scheduling data was generated by CASM 34.2.CASM was run in Phase II mode.(Tic-Visit
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