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Please specify your scheduling constraints or 'No Constraints' on all Observation forms.
Wavelength is a required field.
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Please specify your scheduling constraints or 'No Constraints' on all Observation forms.
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Please specify your scheduling constraints or 'No Constraints' on all Observation forms.0Assigned ID: 2
----- Attempting Submission 1 (Fri Feb 20 21:45:48 GMT 2015) -----joint hst/XMM for Cycle 23 from XMMFor the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/PEAKXD.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/PEAKXD.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/PEAKXD.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/PEAKXD.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/PEAKXD.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/PEAKXD.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/PEAKXD.Submitting on behalf of the PI, Ehud Behar <behar@physics.technion.ac.il>.
Please note coordinated observation with XMM-Newton coming up in May or June.-2131260977----- Attempting Submission 1 (Fri Mar 06 17:12:19 GMT 2015) -----Each grating has at least 4 combinations of central wavelength settings plus FP-POS settings. This is sufficient.
The target has been observed and acquired numerous previous times successfully using these coordinates from the GSC.Tracking Down the Ionized Outflow of NGC 7469Using a multiwavelength campaign on NGC 7469, led by XMM-Newton, HST, Swift, NuSTAR, and optical, we propose to achieve new physical insights into the enigmatic AGN winds, by obtaining the deepest ever RGS spectrum of this highly- accreting source. It will allow us to determine the accurate ionisation and chemical structure of the wind. Using EPIC and RGS, we will measure the response of the outflow to continuum variations, which combined with HST/COS data will unambiguously determine the location, and abundances of the outflow components. Our team pioneered this approach, and applied it successfully (14 refereed papers) to Mrk 509 that featured only a multi-year response. The unique properties of NGC 7469 make it the ideal candidate to respond on shorter, better-monitored time scales.NGC-7469 shows far-UV continuum variations of 17% (rms) over time scales of days to months (Dunn et al. 2006). Historically from HST observations, the UV absorption troughs in NGC-7469 exhibit strong variations in depth as the continuum flux changes (Scott et al. 2005). We expect a roughly linear response for the column density of Ly alpha, NV, and CIV in response to continuum changes. To be sensitive to changes in the absorption lines at the 3-sigma level, a conservative estimate of the required S/N per resolution element is 3/0.17=17.6.
For Ly alpha and NV we will use grating G130M, with FP-POS positions 3 and 4 at a central wavelength setting of 1291, and FP-POS positions 1 and 2 at a central wavelength setting of 1309. This places the detector gap well beyond the N V emission line, and enables us to sample the shortest possible wavelengths down to 1132 A, thus also covering PV 1118,1124, and bridging the gap between detector segments A and B with our two wavelength settings. The four FP-POS positions will permit us to effectively remove detector artifcats and flat-field non-uniformities. We will use grating G160M to cover the C IV line. To place the detector gap redward of the peak in the C IV line (and to avoid the blue-shifted intrinsic absorption lines), we will use central wavelength settings of 1600, FP-POS=1 and 2, and 1623 with FP-POS=1 and 2.
NGC 7469 is fairly bright, and at its historical maximum flux it is too bright to safely do an imaging target acquisition. We therefore use a spectroscopic target acquisition using G130M at the central wavelength setting of 1291 to match the first exposure in each of our visits. We use a conservative estimate of the exposure time in case the target is faint. We calcualte the exposure time at the minimum flux of 2.7e-14 (Dunn et al. 2006), obtain an exposure time of 1.37 s, and then increase that to 3 s to allow for even fainter potential variations.
NGC-7469 has been observed previously with COS on HST. No field objects are bright enough present any dangers due to over illumination of the COS detector. Likewise, the maximum flux of 7.0e-14 observed historically for NGC-7469 is well below the count-rate threshold for safe COS spectroscopic observations.
ETC IDs:
Target Acq Max (7.0e-14): COS.sa.663779 2692 cts/s on B
Target Acq Min (2.7e-14): COS.sa.663788 1236 cts/s on B; requires 1.37 s for S/N=40.
G130M: At the historical median flux of 4.7e-14 at 1377 A (Dunn et al. 2006) and 2000 s total exposure time, we expect a S/N per resolution element of 25. (ETC ID COS.sp.663800)
G160M: At the historical median flux of 4.7e-14 at 1377 A (Dunn et al. 2006) and 2400 s total exposure time, we expect a S/N per resolution element of 26 at 1525 A. (ETC ID COS.sp.663801)AGN/QUASARS12RegularfalsefalsefalsefalsefalseSUPPORTEDGALAXYACCRETION DISKBLRNUCLEUSSEYFERTWINDThis object was identified in the GSC1 catalog, and coordinates were updated to GSC2/ICRS.J2000f(1370 A)=4.7e-14COS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160MCOS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160MCOS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160MCOS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160MCOS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160MCOS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160MCOS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160M/Users/gak/proposals/XMM_2014/phase2/OP-cache/14054v2-v01.xmlThe scheduling data was generated by CASM 23.0.CASM was run in Phase II mode.To be coordinated with an XMM-Newton observation.
The observation is yet to be scheduled in May or June 2015.
The XMM observation will be 80 ks in length (approximately one day), and the HST visit should be within 1 day or less of the XMM observation.(Tic-Visit
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The observation is currently scheduled for XMM rev 2923, 2015-11-24T07:42:47Z to 2015-11-26T07:36:33Z.
The XMM observation will be 80 ks in length (approximately one day), and the HST visit should be within 1 day or less of the XMM observation.(Tic-Visit
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The observation is currently scheduled for XMM rev 2933, 2015-12-14T06:40:07Z to 2015-12-16T06:33:41Z.
The XMM observation will be 80 ks in length (approximately one day), and the HST visit should be within 1 day or less of the XMM observation.(Tic-Visit
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The observation is currently scheduled for XMM rev 2937, 2015-12-22T06:12:32Z to 2015-12-24T06:06:12Z.
The XMM observation will be 80 ks in length (approximately one day), and the HST visit should be within 1 day or less of the XMM observation.(Tic-Visit
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The observation is currently scheduled for XMM rev 2938, 2015-12-24T06:06:12Z to 2015-12-26T06:00:26Z.
The XMM observation will be 80 ks in length (approximately one day), and the HST visit should be within 1 day or less of the XMM observation.(Tic-Visit
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The observation is currently scheduled for XMM rev 2940, 2015-12-28T05:54:48Z to 2015-12-30T05:45:00Z.
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