Betelgeuse: An Iconic and Surprising Red Supergiant

POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE Many warnings are for "out of aperture" which we have had before.. we peak up on the star and then offset +/-50mas, +/-25mas, and back to center. The UV size of Betelguese is many times the optical diameter. We are using the STIS small aperture (25 x 100 mas). This program was copied from GO 16655. 1643130575 ----- Attempting Submission 1 (Tue Jun 28 17:25:27 GMT 2022) ----- We are performing a peak up on Betelgeuse with the small STIS aperture (25X100 mas) and then offsetting +/-50 mas, +/-25 mas in addition to the center... this Phase II was copied from cycle 29 where we did the same thing... and reeived all the same error warnings.. Betelgeuse: An Iconic and Surprising Red Supergiant Multiple ultraviolet spectra of the nearby red supergiant, Betelgeuse, using STIS will enable unique spatially resolved measures of photospheric and chromospheric structure and mass inflows and outflows. This follows the historic dimming of the star captured by HST/STIS in 2019-2020, and will probe the unusual atmospheric structure following the dimming event. An HST campaign of 2 cycles will be complemented by multi-frequency photometry, spectroscopy, interferometry and polarimetry at radio, infrared, and optical wavelengths in order to map surface structures and their variability, and the extended outer atmosphere over both the short (420-day) and long, secondary (2000-day) periods of this supergiant. These observations, coupled with detailed modeling and simulations. will probe the structure, dynamics, and mass loss from Betelgeuse to provide crucial insights into the atmospheric physics and wind-driving mechanisms of red supergiants. During Cycle 29 (the first cycle of a two cycle program), we will make 5 visits of 4 orbits each to the red supergiant Betelgeuse; visits spread over the times of target accessibility. Using the smallest aperture (0.025X0.1") of STIS, the NUV-MAMA E230M (2707) setting, we propose to obtain spectra at 5 positions on the ultraviolet image: center peakup, +/-25 mas, and +/-50 mas offsets. Exposure time at center: 2040 sec. Exposure times at +/-25 mas: 2520 - 3000 sec Exposure times at +/-50 mas: 600 sec We plan a tomographic analysis of the absorption line spectra at center, +/-25 mas, so require S/N ~ 50 at those positions. Andrea Dupree (PI): Dupree was PI of the HST proposal that first imaged the surface of Betelgeuse, and subsequent proposals that obtained spatially resolved uv spectra and determined the rotation and the asymmetical motions in the Betelgeuse atmosphere. She used HST/STIS in Cycles 26-28 to document the massive outflow from the chromosphere of the star that led to the formation of dust and subsequent dimming. She will acquire contemporaneous echelle spectra from TRES to complement the results from STELLA. She leads the program design and analysis of the spectra. Co-Investigators Narsireddy Anugu has proposed for time on CHARA/MIRC-X near-infrared interferometer (H-band), so that time-varying structures can be identified. We have received CHARA/MIRC-X time for 28029 September 2021 Tom Calderwood is an experienced observer with photoelectric photometers and contributes his measurements to the AAVSO database. He is focussing on Betelgeuse and the comparison stars we will use with the STEREO CCD images obtained during the summer. Kateryna Kravchenko, Sophie Van Eck, and Alain Jorisson have developed the tomagraphic techniques that will be used on the photospheric spectrum to diagnose motions in layers of the photosphere. Lynn Matthews is an expert in radio interferometric observations of stars and will focus on the VLA observations. Miguel Montarges, Pierre Kervalla, and Emily Cannon: These folks are leading the proposals for ESO time on SPHERE and MATISSE to image Betelgeuse and perform the reduction and analysis. They have experience in the interferometric imaging of supergiant stars. Andreas Quirrenbach is obtaining the infrared spectra with CARMENES mounted on the 3.5-m telescope at Calar Alto Observatory; this spectral region has valuable temperature diagnostics. Gioia Rau is an expert in cool evolved stars and atmospheric modeling of evolved stars, which will be fundamental to the interpretation of these data. She is experienced with HST data analysis and also an expert in interferometric data. Anita Richards is an experienced radio astronomer who has obtained time on e-MERLIN for Betelgeuse observations. Klaus Strassmeier and Tom Granzer operate the STELLA automatic telescope and echelle spectrograph on Tiede in the Canary Islands. They will obtain and reduce the echelle spectra to determine photospheric radial velocities. William Thompson has arranged for the STEREO observations during May-July 2021. They plan to roll the spacecraft out of contact with Earth for 1 hour every week to obtain many images of the Betelgeuse field. STEREO has a CCD with a wide field of view making comparison stars available to determine the magnitude of Betelgeuse when it is unobservable from Earth. We have and continue to recieve these observations. Betelgeuse is getting brighter. Stellar Physics and Stellar Types Stellar Physics and Stellar Types 6 false false true false false false false true PRIMARY 8 true SUPPORTED STAR M III-I This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 1704817434630 Timing link suitability includes constraints ([02 After 01 by 42.0 to 52.0 days]) The scheduling data was generated by CASM 30.3. 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Spiral in 0.1X0.03 aperature. Center point