Assigned ID: 533
----- Attempting Submission 1 (Fri Feb 26 19:38:56 GMT 2010) -----Updated to add acquisitions for both M87 ad NGC1275.
For M87 do a blind offset after the acquisition (assuming it found M87 nucleus
and not HST-1 as the brightest source in the field). This to be confirmed from
data taken for quiescence check. Otherwise will need to change the offsets.
27 June 2011: resubmitted to fix sign error in RA and Dec offsets in Target 6 M87.----- Attempting Submission 1 (Fri Jun 25 12:06:47 GMT 2010) -----
HST Phase II Proposal 12260 (phase2.apt) successfully submitted.
----- Attempting Submission 2 (Fri Jun 25 12:23:32 GMT 2010) -----
----- Attempting Submission 3 (Thu Dec 02 17:08:20 GMT 2010) -----
----- Attempting Submission 4 (Mon Jun 27 10:08:12 GMT 2011) -----There are warnings relating to uncertainty in positions and the lack of an ACQ/SEARCH. The
positions for both sources come from VLBI observations and are known to better than
milliarcsec precision in the ICRS frame. See Ma et al 1998, AJ 116, 516.Probing Intermediate Ionization Gas in the Perseus and Virgo ClustersThe physics of the evolution of X-ray emitting gas in the cores of clusters is now known to be much more complex than the simple cooling model. In order to understand how the observed molecular/atomic and keV components interact we need to probe the full range of gas phases between these components.
We therefore propose deep ultraviolet spectra of the active nucleii in NGC1275 and M87, the central galaxies in the Perseus and Virgo clusters. Discovery of absorption lines from highly ionized species such as CIV and SiIV will provide a sensitive diagnostic of this crucial intermediate phase of the intracluster medium that is not accessible in any other way.We propose high resolution spectroscopy of the active nucleii in NCG 1275 and M87 covering the
absorption doublets of SiIV 1400, CIV 1550 using COS. HST is required because these lines lie
in the ultraviolet part of the spectrum. COS is the instrument selected as it has the best sensitivity
for these observations.
We aim to reach a sensitivity at SiIV and CIV in equivalent width and column density terms
that are at least a factor of ten better than our initial work on NGC1275 with FOS (Johnstone et
al 1995). That work set a 3sigma equivalent width limit of 300mA on the absorption from the CIV
doublet corresponding to a column density of 1 − 2 × 10^14cm−2 in the C3+ ion.
We have used the COS ETC to estimate exposure times. With the G160M gating set to a
central wavelength of 1600A we can observe the SiIV and CIV lines simultaneously. Assuming
a continuum flux density of 10^−15erg cm^−2 s^−1 ^A−1, (appropriate for NGC1275; M87 is about a factor of two brighter; Pogge et al 2000) a flat continuum in F(lambda) and nominal background levels then in a 3 orbit visit (total of 8600 s on source) a signal-to-noise ratio per resolution element of S/N=9.5 and S/N=6.8 is attained at the (redshifted) wavelengths of SiIV and CIV respectively. Using a resolution element of 6 pixels or 73mA this translates to an equivalent width uncertainty of 7.7mA and 10.7mA respectively, or 3sigma upper limits of 23 and 32 mA.
The VPGUESS program (http://www.eso.org/ jliske/vpguess/) is then used to convert these
equivalent width values to uncertainties in ionic column densities, yielding 3 detection upper
limits of 3 × 10^12cm−2 and and 8 × 10^12cm−2 for SiIV and CIV respectively. These column
densities are on the linear part of the curve of growth and are therefore not dependent on line width for reasonable values of thermal broadening. Uncertainties for M87 will be a factor of sqrt(2) tighter.ISM IN EXTERNAL GALAXIES12false0.00.0falsefalsefalsefalseSUPPORTEDGALAXYBCMELLIPTICALPosition is from VLBI from Ma et al 1998, AJ 116, 516
Flux in the M87 nucleus at ~2700A (ACS/F250W) =0.14mJy (~7e-16 erg/sm/sm/s/A) on 2006 Dec 30 published by Madrid 2009, ApJ 137, 3864 is used for the NUV acquisition exposure time calculation.NGC4486J2000J20002 +/- 0.4 e-15erg/cm^2/s/A at 1600AGALAXYBCMELLIPTICALPosition is from VLBI from Ma et al 1998, AJ 116, 516
Flux at 1600 (FOS 0.21x1.23 aperture) from Johnstone + Fabian 1995 MNRAS 273, 625.
Flux at 2300A confirmed from small extrapolation of preview data for HST dataset O62O05010 (2000-08-18) STIS 52x0.2. That spectrum is largely in agreement with F320W columns in Table 5 of Zirbel + Baum 1998, ApJ, 114, 177 when only point source component is taken into account.J2000J20001+/-0.2 e-15 erg/cm/cm/s/A at 1600A, 3.2e-15 erg/cm/cm/s/A at 2300ACLUSTER OF GALAXIESMULTIPLE NUCLEIOffset to centre COS aperture mid-way betweenM87 nucleus and HST-1. These offsets assume that th acquisition picked up M87 nucleus as the brigher of the two soures. If HST-1 is seen to be brighter than M87 nucleus in the quiescence check observation there offsets need to be changed.J2000COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1600The scheduling data was generated by CASM 19.3.CASM was run in Phase II mode./tmp/OPVisit8249067225015669144.xmlNGC1275(Tic-Visit
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