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the detached m dwarf eclipsing binary tres - her0 - 07621 was published recently as an addition to the few such binary systems previously known @xcite ( see references within , c05 henceforth ) .
this object is interesting because m dwarfs are abundant in our galaxy , and yet are poorly understood .
the binary nature allows us to determine accurate stellar radii and masses .
previously we obtained precise mass estimates of both components of tres - her0 - 07621 ( hobby - eberly telescope , mcdonald observatory ) .
however , due to the 11/pixel resolution of the ccd detectors , our photometric time series is contaminated by a nearby non - variable star , thus providing limitations on the photometric accuracy and precision .
we present some new photometric results based on recently observed non - contaminated time series .
we obtained observations with the _ iac80 _ and _ tcs _ at the observatorio del teide , tenerife and with _ not _ at the observatorio roque de los muchachos , la palma .
the data were reduced using standard reduction procedures and we performed aperture photometry to obtain the time series .
we observed a total of 10 light curves in various filters at 6 different minimum epochs .
we tested to make sure that there were no phase shifts of minimum with filter ( we also found no depth dependance ) .
each of these light curves were fit to a binary system model to obtain the eclipse minima . to obtain a more accurate photometric period , we used the first observed eclipse by stare ( 2003 ) and the quoted hjd from c05 , along with the new minima .
we fit a straight line to the hjd of observed minimum times as a function of elapsed orbital cycle .
the slope of this line gave a period of 1.120804 ( @xmath0 0.000012 ) .
table 1 shows the new eclipse minima for both primary and secondary eclipses .
[ table : observations ]    lcccc hjd & error & cycle no .
& eclipse & observed with + 2452766.5161 & 0.0001 & 0 & 2 & @xmath1 stare + 2453139.74951 & 0.000001 & 333 & 2 & @xmath1 iac80 + 2453503.4368 & 0.0008 & 657.5 & 1 & @xmath1 not + 2453503.4362 & 0.001 & 657.5 & 1 & @xmath2 not + 2453523.6108 & 0.001 & 675.5 & 1 & @xmath3 tcs + 2453527.5333 & 0.001 & 679 & 2 & @xmath3 tcs + 2453536.4999 & 0.0004 & 687 & 2 & @xmath1 not + 2453536.4995 & 0.0004 & 687 & 2 & @xmath2 not + 2453554.4313 & 0.0006 & 703 & 2 & @xmath1 iac80 + 2453554.4306 & 0.0006 & 703 & 2 & @xmath4 iac80 + 2453555.5533 & 0.0004 & 704 & 2 & @xmath1 iac80 + 2453555.5529 & 0.001 & 704 & 2 & @xmath4 iac80 +    we used the data from not to model the binary system ( figure 1 ) . with this higher precision photometry
we have obtained better estimates for both radii , inclination and effective temperature ratio ( table  2 . )    [ table : param ]    lrclr r@xmath5(r@xmath6 ) & 0.449(0.030 ) & & r@xmath7 & 0.449(0.030 ) + m@xmath5(m@xmath6 ) & 0.493(0.003 ) & & m@xmath7 & 0.489(0.003 ) + @xmath8(@xmath9 ) & 83.10(0.30 ) & & t@xmath7/t@xmath5 & 0.97(0.02 ) +
we have provided new minima times and a refined photometric period for the eclipsing binary system tres - her0 - 07621 .
we have also obtained better radii estimates .
we hope that this system will contribute to learning more about low mass stars , there is a lack of such systems observed and so any new ones are not only of benefit but necessary in order to advance in this area of stellar physics .
acknowledgements + thank you to iac80 and tcs at the observatorio del teide , tenerife and not at the observatorio roque de los muchachos , la palma ( spain ) for observing time and their knowledgeable staff : john telting , erik stempels ( not ) , jos miguel gonzlez prez , alfred rosenberg , luis lpez martn ( ot ) .
thanks to peter hammersley for help with the ir data processing .
thanks to travis metcalfe and chris sterken for their suggestions regarding this work .
tres - her0 - 07621 is a recently discovered detached m dwarf eclipsing binary system . 
 we present some follow - up observations of this system including new minima times and a refined orbital period . 
 we have also obtained better estimates of the stellar radii and inclination .