Journal of spectropolarimetric observations of SN 2012aw.
|Epoch||Day(a)||UT Date(b)||MJD(c)||Exposure(d)||Air Mass(e)||Seeing(f)|
|1||16.110||2012-04-01.200||56 018.200||1600 (4)||1.39–1.55||1.2|
|2||45.954||2012-05-01.044||56 048.044||800 (1)||1.24–1.25||1.2|
|3||62.987||2012-05-18.077||56 065.077||6955 (13)||1.27–2.17||1.0|
|4||71.945||2012-05-27.037||56 074.037||7200 (9)||1.26–1.80||1.0|
|5||91.945||2012-06-16.035||56 094.035||4860 (9)||1.33–1.49||1.2|
|6||107.913||2012-07-02.003||56 110.003||3200 (8)||1.65–2.76||1.0|
|7||120.009||2012-07-14.988||56 122.988||1200 (3)||2.25–2.85||2.5|
Notes. All observations were obtained at the VLT using the 300 line/mm grism (“GRIS_300V”) along with the “GG435” order-sorting filter to prevent second-order contamination. This resulted in a useable spectral range of 4350 Å–9200 Å. All observations were made through a 1.′′0 slit, which delivered a resolution of ~12 Å, as derived from the FWHM of night-sky lines. The flux standard used for all observations was BD+26°2606 (Oke & Gunn 1983), observed on the same nights as the science observations. All observations were made with the position angle of the spectrograph slit set to 0 deg, which often differed significantly from the parallactic angle (Filippenko 1982); when coupled with the relatively narrow slit used, the potential for differential light loss – and, hence, inaccurate relative flux calibration – is significant. (a) Day since estimated explosion date of 2012-03-16.09 UT = MJD 56002.09 = JD 2456002.09; Bose et al. 2013). (b) yyyy-mm-dd, calculated as the midpoint of all of the individual exposures. (c)Modified Julian Date(Julian Date – 2400000.5), at the midpoint of all of the individual exposures. (d) Total exposure time in seconds, with the number of complete sets of four waveplate positions obtained shown in parenthesis. (e) Air mass range for each set of observations. (f)Average value of theFWHM of the spatial profile for each epoch, rounded to the nearest 0.′′ 1.
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