M type stars

According to (Cohn et al. 2010):

The fairly high R-band flux indicates that the secondaries are relatively massive, \(\approx 0.5-0.7 \, M_{\odot}\)._

This would mean that the companion star is either an M or K type star. If it is an M type star we should be able to see some Titanium lines. To see what magnitude they have I searched in the public MUSE data release of the Globular Cluster (http://muse-vlt.eu/science/globular-cluster-ngc-6397/). The stars have the id from the ACS Survey if Globular Clusters (Anderson et al. 2008). I searched in this catalog for the right V-I in the VEGA System magnitude. I found some values in the website Intrinsic Johnson-Cousins UBVI Colors of M Dwarf Standard Stars.

In there data I was able to find 8 M stars in the data. The code to find the M stars is the folder scripts/misc/Spectra/Mstars.

The 8 found M stars are:

python ['./pointing32_2014-07-27/ngc6397id000005965jd2456866p5198f002.fits', './pointing24_2014-07-26/ngc6397id000013685jd2456865p6268f000.fits', './pointing23_2014-07-27/ngc6397id000009200jd2456866p5029f002.fits', './pointing22_2014-07-26/ngc6397id000003913jd2456865p6209f002.fits', './pointing12_2014-07-29/ngc6397id000008220jd2456868p6022f002.fits', './pointing34_2014-07-26/ngc6397id000014834jd2456865p6115f000.fits', './pointing51_2014-08-01/ngc6397id000000308jd2456871p6149f000.fits', './pointing31_2014-08-01/ngc6397id000000963jd2456871p6333f002.fits']

The third one is a bit weird so we get the fluxes for the other 7 in the same filters R and H\(\alpha\) for Hubble.

Variability and Magnitudes in the CVs

The basecode is called flux.py and it is in the /scripts/misc/Spectra/fitting folder.

These are the results along in the numbers from (Cohn et al. 2010) and (Kaluzny et al. 2006).

The data

M stars

for i in a:
iraf.wspectext(i, 'M'+i.split('d')[1].replace('0','')+'spectra.txt', header=False)`

import flux
Again the ID is from the [@anderson_acs_2008]
cvU17={'name':'U17','R':flux.getflux('U17','f625w'), 'Halpha':flux.getflux('U17','f658n')}
cvU23={'name':'U23','R':flux.getflux('U23','f625w'), 'Halpha':flux.getflux('U23','f658n')}
cvU19={'name':'U19','R':flux.getflux('U19','f625w'), 'Halpha':flux.getflux('U19','f658n')}
cvU10={'name':'U10','R':flux.getflux('U10','f625w'), 'Halpha':flux.getflux('U10','f658n')}
cvU21={'name':'U21','R':flux.getflux('U21','f625w'), 'Halpha':flux.getflux('U21','f658n')}
cvU25={'name':'U25','R':flux.getflux('U25','f625w'), 'Halpha':flux.getflux('U25','f658n')}
M13685j={'name':'M13685j','R':flux.getflux('M13685j','f625w'), 'Halpha':flux.getflux('M13685j','f658n')}
M14834j={'name':'M14834j','R':flux.getflux('M14834j','f625w'), 'Halpha':flux.getflux('M14834j','f658n')}
M38j={'name':'M38j','R':flux.getflux('M38j','f625w'), 'Halpha':flux.getflux('M38j','f658n')}
M3913j={'name':'M3913j','R':flux.getflux('M3913j','f625w'), 'Halpha':flux.getflux('M3913j','f658n')}
M5965j={'name':'M5965j','R':flux.getflux('M5965j','f625w'), 'Halpha':flux.getflux('M5965j','f658n')}
M822j={'name':'M822j','R':flux.getflux('M822j','f625w'), 'Halpha':flux.getflux('M822j','f658n')}
M963j={'name':'M963j','R':flux.getflux('M963j','f625w'), 'Halpha':flux.getflux('M963j','f658n')}

Problems

Maybe I need to cut VEGa to fit my observation. I dont know. I am getting a Halpha flux bigger than the R flux and it should be like that. Ti is a narrow vs wide field