A UV spectroscopic snapshot survey of low-mass stars in the Hyades
Because of its proximity, the 650-Myr-old Hyades open cluster is a unique resource for exploring the relationship between magnetic activity, rotation, and age in low-mass stars. While the cluster has been largely ignored in UV studies of the dependence of activity on rotation, we now have an extensive and growing set of complementary rotation period, Halpha, and X-ray measurements with which to examine in detail the rotation-activity relation at 650 Myr and to constrain theories of magnetic heating. We propose to measure Mg II line emission, the strongest NUV activity tracer, in COS spectra of 86 Hyads ranging in spectral type from G to M with known rotation periods or currently being observed by K2. These stars form a representative sample of low-mass Hyads with known periods and are a significant addition to, and expansion of, the sample of 20 mainly solar-mass rotators with existing (mostly low-resolution) IUE NUV spectra. The Mg II measurements will contribute significantly to our goal of mapping out the rotation-activity relation star-by-star in this benchmark open cluster. This, in turn, will move us toward an improved understanding of the radiation environment and habitability of the exoplanets we continue to find around low-mass stars.
We select two groups of SNAP targets. With the first group, our focus is on completely characterizing the low-mass Hyads for which we have a measured rotation period and Halpha and X-ray data, a total of 75 <1.1 Msun stars. Twenty of these stars have existing IUE spectra, and we are therefore left with 55 stars for which we require HST NUV spectroscopy. We then select additional Hyades SNAP targets that have previously measured periods but no X-ray detections, as well as stars from our approved target list for K2 Campaign 13. While the K2 targets do not have measured periods yet, based on our analysis of Campaign 4 data we will measure periods for ~80% of them (Douglas et al. 2016).
To compute the exposure times for these targets, we need to select an input spectral energy distribution and magnitude. For G stars, we use the default Bruzual synthetic stellar spectra provided by the COS ETC. For K1 to M5 stars, we input MUSCLES SEDs into the ETC, since these are based in part on HST UV spectra (Loyd et al. 2016), and model spectra for these stars are known to underestimate the chromospheric contribution to the UV.
Thirty SNAP targets have GALEX NUV magnitudes, and we use these to compute the exposure times for these stars. For the remaining stars, we use the 356 cluster members with GALEX NUV detections to estimate average absolute NUV magnitudes as a function of spectral type. We then find the appropriate absolute NUV magnitude for each target based on spectral type, and convert these to apparent NUV magnitudes. Comparisons between our estimated NUV magnitudes for those targets that also have measured GALEX NUV magnitudes indicate that the estimated NUV magnitudes are reasonable. For solar-mass stars, our estimated magnitudes are systematically too bright by ~0.5 magnitudes, while for early M dwarfs our estimates are too conservative by roughly the same amount. For mid-M dwarfs, our estimated NUV magnitudes are again too bright, and so to be conservative we add a 0.5 magnitude to the NUV magnitudes we derive to calculate their exposure times.
The results of this procedure warrant a two-pronged approach: for 19 targets, the required exposures correspond to at least one HST orbit, and 17 of those targets were included in a separate GO program (15090). For 86 other targets, a snapshot program is more appropriate, and those are the targets listed here.
To finalize our observing strategy, we followed Instrument Science Report COS 2017-01 to assess the safety of observing our M-dwarf targets. This is a multiple-step process: first, we obtained a spectral type for our targets. For most stars this was done directly from our MDM spectra; for others we converted absolute K magnitudes into spectral types, following the relations laid out in Kraus & Hillenbrand (2007). These spectral types were converted into (U-V) colors using the data presented in Pecaut & Mamajek (2013). We then searched the literature for V magnitudes for our targets; for stars lacking a V in the literature, we computed one from e.g., Sloan Digital Sky Survey (g-r) colors. We combined these V magnitudes with the (U-V) color to obtain the U magnitudes needed to characterize the potential impact of flares on our observations. Our comparisons of these U magnitudes to those in the literature for our targets that have U-band measurements indicate that our derived U magnitudes have uncertainties ~0.3-0.5 magnitudes.
Finally, we used our MDM spectra to determine whether, based on their measured Halpha EqWs, our targets are magnetically active. This sets the maximum U-band magnitude increases (Delta U) of the brightest flare that would occur with a probability of 10^-4. We then computed U_{flare} = U_{quiescent} + Delta U and determined global and local count rates for a flare of this magnitude using COS ETC calculations for the NUV. All of our targets are well below the count-rate limits for the COS photon-counting detectors.
Our instrumental set-up is as follows: we wish to observe our targets using COS in low-resolution mode with the G230L grating. Centered at 2950 A, the resulting spectra will cover the Mg II h and k lines, which are the strongest NUV tracers of magnetic activity. We set up the exposure in ACQ/IMAGE mode, requesting S/N = 40 in the COST ETC. For targets that are bright enough to generate count warnings in the MIRROR A + PSA configuration, we set MIRROR B + PSA, or MIRROR A + BOA, as the combination for image acquisition. We use TIME-TAG mode for the actual observation of each target and set FP-POS = 4. The exposure times we calculate insure that we have a S/N > 10 in the Mg II lines, which based on the IUE spectra is what is requred to measure these lines confidently, and a S/N > 5 (and generally also close to 10) for the nearby continuum, based on the input spectra/SEDs.
Stellar Physics
6
false
SUPPORTED
STAR
G V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
14.36
STAR
K V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
14.52
STAR
K V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
16.16
STAR
K V-IV
NO
J2000
15.56
STAR
K V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
15.53
STAR
K V-IV
NO
J2000
15.12
STAR
K V-IV
NO
J2000
15.67
STAR
K V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
15.71
STAR
K V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
15.70
STAR
K V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
16.01
STAR
K V-IV
NO
J2000
16.08
STAR
K V-IV
NO
J2000
16.36
STAR
K V-IV
NO
J2000
16.51
STAR
K V-IV
NO
The Gaia 2018 data release includes a position for this star with relatively large uncertainties (04 26 48.2672 +10 52 15.94, 0.3573 0.2760). The 2MASS position is therefore the one quoted here.
J2000
16.92
STAR
K V-IV
NO
Proper motion updated to reflect Gaia 2018 data release. The 2018 Gaia position has (relatively) large uncertainties (04 40 25.4307 +16 30 49.3975, 0.5398 0.2054), presumably due to binary nature of this star, which is not something first two data releases handle well, so the position is (still) from 2MASS.
J2000
16.51
STAR
K V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
16.31
STAR
K V-IV
NO
J2000
16.77
STAR
K V-IV
NO
J2000
17.46
STAR
K V-IV
NO
J2000
17.10
STAR
K V-IV
NO
J2000
17.87
STAR
K V-IV
NO
J2000
16.88
STAR
K V-IV
NO
Position updated to Gaia DR2 values. Proper motions updated to Gaia DR1 values.
J2000
17.07
STAR
K V-IV
NO
J2000
17.35
STAR
K V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
17.59
STAR
K V-IV
NO
J2000
18.64
STAR
M V-IV
NO
J2000
18.67
STAR
K V-IV
NO
J2000
19.07
STAR
K V-IV
NO
Position and proper motion updated to reflect Gaia 2018 & 2016 data releases, respectively.
J2000
19.01
STAR
K V-IV
NO
Position and proper motion updated to reflect Gaia 2018 data release.
J2000
19.11
STAR
K V-IV
NO
Position and proper motion updated to reflect Gaia 2018 data release.
J2000
18.53
STAR
K V-IV
NO
Position and proper motion updated to reflect Gaia 2018 data release.
J2000
18.88
STAR
K V-IV
NO
Position and proper motion updated to reflect Gaia 2018 data release.
J2000
19.18
STAR
K V-IV
NO
J2000
19.43
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
19.66
STAR
M V-IV
NO
J2000
18.60
STAR
M V-IV
NO
J2000
18.69
STAR
M V-IV
NO
J2000
20.04
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
19.49
STAR
M V-IV
NO
J2000
19.98
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
19.79
STAR
M V-IV
NO
J2000
19.52
STAR
M V-IV
NO
J2000
18.88
STAR
M V-IV
NO
J2000
20.40
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
19.74
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
18.59
STAR
M V-IV
NO
J2000
19.76
STAR
M V-IV
NO
J2000
19.29
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
20.28
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
19.90
STAR
M V-IV
NO
J2000
20.90
STAR
M V-IV
NO
Position and proper motion updated to reflect Gaia 2018 data release.
J2000
20.12
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
19.82
STAR
K V-IV
NO
J2000
19.42
STAR
M V-IV
NO
J2000
20.21
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
21.74
STAR
M V-IV
NO
Position and proper motion updated to reflect Gaia 2018 data release.
J2000
20.88
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
20.36
STAR
M V-IV
NO
J2000
21.46
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
19.94
STAR
K V-IV
NO
Position and proper motion updated to reflect Gaia 2018 data release.
J2000
19.49
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
19.58
STAR
M V-IV
NO
J2000
20.32
STAR
K V-IV
NO
Position and proper motion updated to reflect Gaia 2018 data release.
J2000
19.70
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
19.31
STAR
K V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
16.22
STAR
K V-IV
NO
Position updated to Gaia DR2 values. Proper motion is from Gaia DR1.
J2000
16.57
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
19.31
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
20.47
STAR
M V-IV
NO
J2000
19.05
STAR
K V-IV
NO
J2000
17.44
STAR
M V-IV
NO
J2000
20.84
STAR
K V-IV
NO
Position updated to reflect Gaia 2018 data release.
J2000
18.87
STAR
K V-IV
NO
Position and proper motion updated to reflect Gaia 2018 data release.
J2000
19.71
STAR
K V-IV
NO
J2000
16.96
STAR
M V-IV
NO
No Gaia data available.
J2000
18.77
STAR
M V-IV
NO
J2000
20.6373653
STAR
M V-IV
NO
J2000
20.9324284
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
21.07
STAR
M V-IV
NO
No Gaia data, presumably because it is a known binary.
J2000
21.32
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
21.73
STAR
M V-IV
NO
Position and proper motions updated to Gaia DR2 values.
J2000
20.86
COS/NUV
Spectroscopic
No
No
G230L
2950
COS/NUV
Spectroscopic
No
No
G230L
2950
COS/NUV
Spectroscopic
No
No
G230L
2950
COS/NUV
Spectroscopic
No
No
G230L
2950
COS/NUV
Spectroscopic
No
No
G230L
2950
COS/NUV
Spectroscopic
No
No
G230L
2950
COS/NUV
Spectroscopic
No
No
G230L
2950
COS/NUV
Spectroscopic
No
No
G230L
2950
COS/NUV
Spectroscopic
No
No
G230L
2950
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(Tic-Orbit
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:si-vis-utilization 921
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:internal-dur-at-end 331
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3156
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Orbit
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:internal-dur-at-end 331
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:pcs-visibility 3149
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)
false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Orbit
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false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=11.70
Target switched to STIS.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Orbit
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Orbit
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false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=11.30
Target switched to STIS.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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)
false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=13.30
Target switched to G230MB, following suggestion from Joleen Carlberg to address issue with previous configuration violating bright object constraints. E1 pseudo-aperture location selected to address CTE warning in previous configuration.
The scheduling data was generated by CASM 27.2.
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(Tic-Visit
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
1
0
The scheduling data was generated by CASM 27.2.
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(Tic-Visit
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)
false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=14.90
Target switched to STIS.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=14.00
Target switched to G230LB, following suggestion from Joleen Carlberg to address issue with previous configuration violating bright object constraints. E1 pseudo-aperture location selected to address CTE warning in previous configuration.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3165
:pcs-gap 0
)
false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=11.60
Target switched to STIS.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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:pcs-visibility 3156
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)
false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=15.90
Target switched to STIS.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=14.30
Target switched to STIS.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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:max-dark-utilization 1920
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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)
false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=12.30
Target switched to STIS.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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:max-dark-utilization 1920
:low-sky "N"
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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:internal-dur-at-end 331
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:dark-utilization 0
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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:internal-dur-at-end 331
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:dark-utilization 0
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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:internal-dur-at-end 331
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:max-dark-utilization 1920
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:pcs-visibility 3149
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Orbit
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:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)
false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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:data-volume 69760
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(Tic-Orbit
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:internal-dur-at-end 341
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3156
:pcs-gap 0
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false
1
0
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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:pcs-gap 0
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false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=15.53
Target switched to STIS.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=15.16
Target switched to STIS.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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)
false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=15.35
Target switched to STIS.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=15.00
Target switched to STIS.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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:visit-id "84"
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false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=15.02
Target switched to STIS.
The scheduling data was generated by CASM 27.2.
CASM was run in Phase II mode.
(Tic-Visit
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:dark-utilization 0
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:low-sky "N"
:pcs-visibility 3165
:pcs-gap 0
)
false
1
0
Target switched to STIS. ACQ done with longpass filter and exposure time calculated using V=13.67
Target switched to G230LB, following suggestion from Joleen Carlberg to address issue with previous configuration violating bright object constraints. E1 pseudo-aperture location selected to address CTE warning in previous configuration.