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RESCHEDULED:
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MUSCLES Treasury Survey - Spectra of M & K Exoplanet Host Stars
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PI: Kevin France (Colorado) | ||
MUSCLES Series: | ||
MUSCLES Paper I - France et al. 2016, ApJ, 820, 89 | MUSCLES Paper IV - Youngblood et al. 2017, ApJ, 843, 31 | |
MUSCLES Paper II - Youngblood et al. 2016, ApJ, 824, 101 | MUSCLES Paper V - Loyd et al. ApJ, submitted | |
MUSCLES Paper III - Loyd et al. 2016, ApJ, 824, 102 | ||
Semi-Empirical Synthetic Models: | ||
Fontenla et al. 2016, ApJ, 830, 154 |
Introduction |
Data Products |
Data Access |
Plot Scripts |
README (TXT) (PDF) |
Acknowledgement: If you make use of the MUSCLES spectral data products, please cite Papers I, II, and III from the top of this page and specify the version number of the spectra you used in your work. The version number is in the filenames. For example, "v22" denotes version 2.2. If you use the semi-empirical synthetic models, please cite the relevant paper(s) in the "Semi-Empirical Synthetic Models" section at the top of the page. |
MUSCLES is a spectral survey of 11 low-mass, planet-hosting stars, 7 M and 4 K dwarfs. The spectra cover wavelengths from 5 Å to 5.5 µm, with emphasis on high-energy radiation. More information on the MUSCLES survey and collaboration can be found at the MUSCLES team page. Data sources for the various regions of the spectra are:
The data products from each of the 11 stars are organized into subdirectories based on the star name. Several files are available for each target. We provide a brief summary below, for full details, consult the README file.
Primary Data Products
Ancillary Data Products
In response to popular demand after the announcement of the discovery of a habitable-zone planet orbiting Prox Cen, we added Prox Cen to the MUSCLES sample and created an SED from archival data using methodology consistent with the other MUSCLES SEDs. We highly encourage users of the Prox Cen spectra to read these notes on the reduction of the Prox Cen spectra, as they address an important issue regarding the stellar effective temperature and bolometric flux.
Also available for download is a synthetic spectrum of the MUSCLES M2 dwarf GJ 832 from Fontenla et al. 2016. The synthetic spectrum was created from a one-dimensional model of the stellar atmosphere that incorporates non-LTE radiative transfer techniques and many molecular lines. The synthetic spectrum covers 1 Å - 1 mm at a resolving power R = 100,000 (denoted by "r1e5" in the file names). A single resolution element equals two wavelength samples. For consistency with the MUSCLES data products, the synthetic spectrum's wavelength is in Angstroms and the flux is reported as would be observed from Earth (erg/cm2/s/Å) under the assumption that the stellar radius = 0.499 R_solar (Houdebine 2010) and distance = 4.95 pc (van Leeuwen 2007). Note that Houdebine et al. 2016 determine GJ 832's stellar radius to be 0.458 ± 0.039 R_solar. The atomic and molecular transitions appear at their laboratory rest wavelengths (vacuum). Semi-empirical models of the other 10 MUSCLES stars as well as Proxima Centauri and TRAPPIST-1 are coming soon. If you utilize the GJ 832 synthetic spectrum, please cite Fontenla et al. 2016, ApJ, 830, 154.
Click on a star name to visit the Simbad page for that target. Download a .tar.gz containing all FITS files for a target using the (tar) link.
Click on "FITS" to directly download the FITS file. Click on "PL" to use the MAST interactive plotter.
Note: The STIS observations used a few different modes for a given central wavelength, e.g., the _140_ column contains spectra observed with either the G140M or E140M modes. In all cases, consult the FITS header and/or file name to get the full observation modes used for a given target.
NOTE: The X-ray spectrum for HD 97658 does not come from XMM or Chandra observations. It is scaled from X-ray data of HD 85512, which shows similar lines in the UV. For more details, consult the README or primary publication.
Target | XRAY | EUV | FUV-NUV-VIS | MIR | FIR-SUBMM | ALL | |
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(1-100 Å) | (100-912 Å) | (912 Å - 2.5 μm) | (2.5 - 500 μm) | (500 μm - 1 mm) | |||
  | R = 100,000 | R = 100,000 | R = 100,000 | R = 100,000 | R = 100,000 | R = 100,000 | |
GJ 832 | FITS PL | FITS PL | FITS PL | FITS PL | FITS PL | FITS PL |
The example file used here, hlsp_muscles_multi_multi_gj436_broadband_v10_adapt-const-res-sed.fits, can be downloaded by clicking the "FITS" link in the GJ 436 / Adaptive Res row under the Panchromatic / Const column.
Python:
from astropy.io import fits import matplotlib.pyplot as plt spec = fits.getdata('hlsp_muscles_multi_multi_gj436_broadband_v10_adapt-const-res-sed.fits',1) plt.plot(spec['WAVELENGTH'],spec['FLUX']) plt.xlabel('Wavelength (Angstroms)') plt.ylabel('Flux Density (erg/cm2/s/Ang)') plt.show()
data_436 = MRDFITS(path+'hlsp_muscles_multi_multi_gj436_broadband_v10_adapt-const-res-sed.fits',$ 1,head_436) wave = data_436.wavelength flux = data_436.flux error = data_436.error plot, wave, flux, xs=1, ys=1, xr=[10,50000], yr=[0.001,10000]*1d-15,$ /ylog, /xlog, TITLE='GJ 436; MUSCLES Example',$ xtitle='Wavelength (Ang)', ytitle='Observed Flux Density (erg/cm2/s/Ang)',$ charsize=1.75
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