0Assigned ID: 326
----- Attempting Submission 1 (Thu Apr 06 22:48:16 GMT 2017) -----
HST Phase I Proposal 326 (Mdwarf.apt) successfully submitted.
Receipt: # 326-1
----- Attempting Submission 2 (Fri Apr 07 14:33:42 GMT 2017) -----
HST Phase I Proposal 326 (Mdwarf.apt) successfully submitted.
Receipt: # 326-2Update Phase II to extend "BETWEEN" dates through 2020.
Redo Phase II with new APT version.185550075----- Attempting Submission 1 (Fri Jul 14 20:04:03 GMT 2017) -----
HST Phase II Proposal 15326 (Mdwarf.apt) successfully submitted.
Receipt: # 15326-1
----- Attempting Submission 2 (Thu Aug 17 21:54:55 GMT 2017) -----
----- Attempting Submission 3 (Wed Jan 02 16:59:27 GMT 2019) -----Characterizing the Winds of M Dwarf StarsWe propose to use HST/STIS to study the H I Lyman-alpha spectra of nine very nearby (d<7 pc) M dwarf stars, to measure stellar mass-loss rates using the astrospheric absorption technique. The Lyman-alpha astrospheric absorption signature is currently the only means of detecting the coronal winds of cool main sequence stars, and HST is the only observatory that has ever been capable of observing it. Our goal is to use the absorption to study the winds of M dwarf stars, and for the first time characterize how these winds correlate with stellar activity, as quantified by X-ray luminosity. Astrospheric absorption has so far been observed for only one M dwarf (EV Lac), so our project will greatly increase our understanding of M dwarf winds. Our measurements will be compared with and test predictions for M dwarf wind behavior from theoretical/numerical models, and from studies of stellar angular momentum evolution. We will also investigate the implications that our measurements have for planets orbiting M dwarfs.We plan to observe 9 M dwarfs stars with STIS for 4 orbits each. Our project is focused on detecting and measuring astrospheric absorption in the H I Lyman-alpha line at 1216 Angstroms, using the E140M grating, but confidence in this analysis is significantly improved with information provided by observations of the Mg II h & k lines near 2800 Angstroms, so we also be observe the Mg II lines using the E230H grating. We acquire each of our rather bright stars with a short exposure onto the STIS/CCD with the F28X50OII filter. An accurate wavelength scale is important for our purposes so we perform a peakup into the narrow 0.2X0.05ND aperture. This neutral density aperture is required to reduce the flux for our bright targets.
After acquisition and peakup, we spend the first orbit obtaining the E230H spectrum of the 2574-2851 Angstrom wavelength range, through the 0.2x0.09 aperture. The remaining 3 orbits are spent observing the 1150-1700 Angstrom range with the E140M grating, through the 0.2x0.2 aperture. The E140M grating does not have quite the resolution of E230H, but its R= 45,800 resolution is good enough to study the H I Lyman-alpha line profile in the detail that we require. Because M dwarfs are known to be variable, we plan on obtaining our spectra in TIME-TAG mode.
Estimating expected S/N for our planned spectra requires first estimating Lyman-alpha and Mg II fluxes, which can be done roughly by extrapolating from previously observed M dwarfs, particularly EV Lac. Chromospheric line fluxes (such as Mg II and Lyman-alpha) are related to X-ray fluxes through known scaling laws (Wood et al. 2005a). Thus, Lyman-alpha or MgII fluxes for our stars can be estimated from known X-ray luminosities of our target stars. We expect our E230H spectra to attain a sufficient signal-to-noise of S/N>15 per resolution element at line center for the strong Mg II lines, and the E140M spectrum to achieve a peak S/N>10 within the H I Lyman-alpha line.
All of our targets are comfortably in compliance with STIS/MAMA bright object limits, as verified using both
Table 13.44 in the STIS Instrument Handbook and the online STIS exposure time calculator. However, there is concern with regards to using COS or STIS to observe stars that flare, as M dwarfs in particular are known to do. A particularly massive flare could in principle violate Bright Object limits, even if the quiescent emission is orders of magnitude below them. Our 7 less active stars with log Lx<28 (see Table 1), which do not show H-alpha in emission, should be considered "inactive" and thereby easily observable based on flare star brightness constraints described in STIS ISR 2017-02. However, our two most active targets, GJ285 (M4.5 Ve) and GJ 644A (M3.5 Ve), which have log Lx>28 and show H-alpha in emission, should be considered "active" and are therefore problematic, as they are in the particularly problematic M3-5 spectral range.
For evaluating the safety of the E230H observation of GJ285 and GJ644A, we model a particularly big flare spectrum following STIS ISR 2017-02, decreasing the star's U magnitude by 8 mags, and then computing the resulting spectrum assuming a T=9000 K blackbody. For both GJ285 and GJ644A, the resulting E230H spectrum does not quite violate the Bright Object constraints, but it is very close.
For evaluating the safety of the E140M observation of GJ285 and GJ644A, it is the Lyman-alpha line that is the line likely to be the source of concern, the continuum being unimportant even for a big flare. And it is the local count rate at the peak of the Ly-alpha line that is most likely to viiolate Bright Object limits. Following STIS ISR 2017-02, we take the aforementioned flare U magnitudes and use them to estimate a C IV flux for the flare using the Hawley et al. (2003) relation, leading to f(CIV)=3.1e-10 and f(CIV)=4.1e-10 ergs/cm2/s for GJ285 and GJ644A, respectively. In order to extrapolate to a Ly-alpha peak flux (in ergs/cm2/s/A), f(Lya), we note that 3 M flare stars previously observed by STIS/E140M (AD Leo, EV Lac, AU Mic) have shown f(Lya)/f(CIV) ratios of 3.1, 6.9, and 9.2, respectively (e.g., Wood et al. 2005). We argue that assuming the maximum of these values, f(Lya)/f(CIV)=9, is a reasonably conservative assumption, noting that during a giant flare the expectation would be that f(Lya)/f(CIV) should if anything go DOWN, as high temperatures are more prevalent during a flare. With this assumption, we compute f(Lya)=2.8e-9 and f(Lya)=3.7e-9 ergs/cm2/s/A for GJ285 and GJ644A, repsectively. Using the STIS ETC, we find that this does not violate the Bright Object constraint, but as for the E230H spectrum, it is very close.Stellar Physics6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARM V-IVNOSee individual measurements in SIMBAD for U-mag.HD217987J2000J2000U-MAG=10.02+/-0.05, TYPE=M2V, F-LINE(2796)=4.7+/-1.2E-13, W-LINE(2796)=0.3, F-LINE(1216)=3.7+/-0.9E-13, W-LINE(1216)=0.9STARM V-IVNOSee individual measurements in SIMBAD for U-mag.HD1326GX-ANDJ2000J2000U-MAG=10.93+/-0.05, TYPE=M2V, F-LINE(2796)=5.0+/-1.3E-13, W-LINE(2796)=0.3, F-LINE(1216)=4.5+/-1.1E-13, W-LINE(1216)=0.9STARM V-IVNOLHS-33J2000J2000U-MAG=12.56+/-0.05, TYPE=M3.5V, F-LINE(2796)=1.5+/-0.4E-13, W-LINE(2796)=0.3, F-LINE(1216)=1.1+/-0.3E-13, W-LINE(1216)=0.9STARM V-IVNOGJ 860 is a close binary (M3+M4) with an orbital period of 44.67 yr, and with the companion (GJ 860B) only ~1.6" away in 2017. Orbital motion will make the coordinates more uncertain. SIMBAD coordinates and V magnitudes are clearly wrong due to the confusion of the two stars, so numbers are taken directly from Hipparcos, which are epoch 1991.25.HD239960AKRUGER-60AJ2000J2000U-MAG=12.52+/-0.10, TYPE=M3V, F-LINE(2796)=3.4+/-0.9E-13, W-LINE(2796)=0.3, F-LINE(1216)=3.7+/-0.9E-13, W-LINE(1216)=0.9STARM V-IVNOHD36395J2000J2000U-MAG=10.63+/-0.05, TYPE=M1.5V, F-LINE(2796)=3.0+/-0.8E-13, W-LINE(2796)=0.3, F-LINE(1216)=2.8+/-0.7E-13, W-LINE(1216)=0.9STARM V-IVNOLHS-397J2000J2000U-MAG=11.92+/-0.05, TYPE=M2.5V, F-LINE(2796)=1.3+/-0.3E-13, W-LINE(2796)=0.3, F-LINE(1216)=1.0+/-0.3E-13, W-LINE(1216)=0.9STARM V-IVNOActive flare star.YZ-CMIJ2000J2000U-MAG=13.76+/-0.05, TYPE=M4.5V, F-LINE(2796)=2.5+/-0.6E-13, W-LINE(2796)=0.3, F-LINE(1216)=3.5+/-0.9E-13, W-LINE(1216)=0.9STARM V-IVNOSee individual measurements in SIMBAD for U-mag.HD79210J2000J2000U-MAG=10.26+/-0.05, TYPE=M0V, F-LINE(2796)=3.6+/-0.9E-13, W-LINE(2796)=0.3, F-LINE(1216)=3.4+/-0.9E-13, W-LINE(1216)=0.9STARM V-IVNOGJ 644 is a messy system consisting of 5 M dwarfs: GJ 644A (M3), GJ 644B a very nearby (~0.2") spectroscopic binary (M4+M4), GJ 643 a distant (~72") M3.5 star, and GJ 644C a very distant (~220") M7 star. SIMBAD magnitudes can't be trusted due to multiplicity. Actual magnitudes found in Mazeh et al. (2001).HD152751WOLF-630AJ2000J2000U-MAG=13.42+/-0.05, TYPE=M3V, F-LINE(2796)=5.1+/-1.3E-13, W-LINE(2796)=0.3, F-LINE(1216)=7.7+/-1.9E-13, W-LINE(1216)=0.9STIS/NUV-MAMASpectroscopicNoNoE230H2713STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230H2713STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230H2713STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230H2713STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230H2713STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230H2713STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230H2713STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230H2713STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230H2713STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230H2713STIS/FUV-MAMASpectroscopicNoNoE140M1425The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode./private/var/folders/0b/qbp4bysx6vdbfxvp_xw3dyxw00023y/T/OPVisit1396832895887043701.xml154467339100073.02072000000001(Tic-Visit
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