This dataset contains Magellan MIKE spectroscopy of a population of cool, luminous stars in the Magellanic Clouds, a sample of confirmed Magellanic Cloud red supergiants, and spectrophotometric standard stars. The spectra were analyzed in the paper "Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds. II: Spectroscopic and Environmental Analysis of Thorne-\.Zytkow Object and Super-AGB Star Candidates" by O'Grady et al. (2022). 

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Spectra naming scheme:

[date]_[name]_[radec]_[red/blue].fits

[date] = One of 201803, 201901, 201912, or 202001, indicating the year and month of the observing run during which the observation was taken. Complete information on the date and time of the observation is contained in the header.

[name] = The name of the star as given in O'Grady et al. (2022). HV 2112 is indicated with hv2112_, HLOs are indicated with smc/lmc#_, HAVs with hav#_, RSGs with rsg#_, and standard stars with stand_[name]_.

[radec] = The right ascension and declination of the object in degrees, e.g. 17.515835-72.614603

[red/blue] = Either 'red' or 'blue', denoting the red and blue arms of MIKE (https://www.lco.cl/?epkb_post_type_1=mike)

Thus the file name for the red arm observation of HV 2112 would be: hv2112_mar2018_17.515835-72.614603_red.fits

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Spectra Description

[1] The spectra have been reduced using the Carnegie Observatories CarPy MIKE reduction pipeline: https://code.obs.carnegiescience.edu/mike
[2] These spectra have not been flux calbirated.
[3] These spectra have not been doppler corrected. Users are free to use the doppler shifts given in O'Grady et al. (2022), or perform their own doppler corrections. ## to the rest frame (not heliocentric correction either). These spectra are in observed frame wavelengths; ./. helio or radial
[4] These spectra have not been manually continuum flattened. While the CarPy reduction pipeline automatically produces a relative fluxing (see 7. below), in our paper we instead normalize smaller chunks of the spectra that were of interest.
[4] These fits files have multiple extensions. From the CarPy MIKE reduction pipeline website, the extensions are:

1. Sum of the sky over the extraction aperture.
2. Sum of the object over the extraction aperture.
3. Expected noise from sum of object and sky plus the read noise.
4. Signal-to-noise spectrum (per pixel).
5. The sum of the lamp spectrum over the extraction aperture. However, this is only from the first lamp exposure since small wavelength
	shifts between lamp and science frames would cause unwarranted blurring of the lamp lines in this extracted spectrum.
6. Flattened-flat, or blaze.
7. Spectra divided by the flattened-flat, or relative fluxing.

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Please cite the linked paper when using this dataset. DOI provided on Zenodo.

Title: Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds. II: Spectroscopic and Environmental Analysis of Thorne-\.Zytkow Object and Super-AGB Star Candidates

Authors: Anna J. G. O‘Grady, Maria R. Drout, B. M. Gaensler, C. S. Kochanek, Kathryn F. Neugent, Carolyn L. Doherty, Joshua S. Speagle, B. J. Shappee, Michael Rauch, Ylva Gotberg, Bethany Ludwig, and Todd A. Thompson
