P Cygni observations


20 17 47.2018 +38 01 58.549

Iron Line Paper (SINFONI HH99)
Single-click images to expand.

The images on this page are proprietary (i.e. you must ask permission to use them), but if anyone is interested I'm open to adding collaborators to this project.

Observations

    NICFPS coronography - October/November 2007
    TripleSpec Spectroscopy - September 5 2008

Inner Nebula



Outer nebula


Radial Profile


Postscript version of the outer nebula image
Postscript version of the inner nebula
Postscript version of the inner nebula in color


20 um Gemini proposal (txt): gemini_proposal.txt
20 um Gemini proposal (pdf): gem_prop.pdf

Michelle work:
Michelle Filters
Michelle calibrators
Michelle Integration Time Calculator
Uniform Surface Brightness: 10 mJy / sq arcsec assumed (no good reason)
Q filter used
70K BB -> 3.53 S/N in 6000s
150K BB -> 5.95 S/N in 6000s
Questions:
Can [FeII] 1.64um emission be used to measure density?
Are different distances measured below real? What do they mean?
Can the radial profile be fit by a model of concentric spherical shells? How can I implement such a model? Is it worth it?
It looks like concentric filled optically thin spheres work better than hollow shells (see last figure)
Important notes:
Inner-outer nebula is approximately continuously filled, but there are some clumps in the outer nebula that are brighter
Therefore the outer nebula is also clumpy
'Inner nebula' has roughly defined radius 12.9" - 14.5"
This is greater than the 7.9"-9.7" in Smith & Hartigan 2006: spectra measure brighter portion of nebula?
Image is probably deeper than spectra
Assuming ejection in 1600 for inner ring:
d=1.7 kpc -> 1" = .008 pc = 2.54e16 cm
r = 14.5" = .12 pc = 3.68e17 cm
r/t = 3.68e12 km / (86400s * 365d * 407yr) = 287 km/s
for r=9.7", v=191 km/s
Making the same assumption for the outer ring (for comparison):
r = 45" (roughly) = .37 pc = 1.14e18 cm
r/t = 890 km/s
Going the other way, assuming ~200 km/s speed, get dynamical age:
Inner (14.5"): 584yr
Outer (45"): 1800yr
Is the radius difference for the inner nebula because of the "blowout" material?
At 200 km/s, 1700 kpc, proper motion ~ .025"/yr (i.e. unobservable over <20-30yr baseline)


Absolute Flux Calibration:
I tried to calibrate by converting the [Fe II] 1.64um star magnitudes to 2MASS H-band.
There are a few sources of error I'm not 100% sure how to deal with:
  1. The background of the final image is not zero and is not perfectly flat (it's approximately -8 with a standard deviation of 22)
  2. The background noise & level in the final image and the image used to calculate the absolute magnitude are very different (mean differs by 21 counts, stdev is a factor of 4 larger in the non-subtracted image).

2MASS H-band filter: ~ .83 * .2um (2MASS filters)
Chip sensitivity over same range: .63 * .2um
However, they claim the total response of the H-band filter is close to 1.... perhaps they include the factor of ~.5 as a gain?
FWHM for [Fe II] 1.64um filter at APO is .0055um. Transmission function is not listed; assume 1 for now.
2MASS zero magnitude flux: H-band 1024 Jy

average magH - magFe = 25.87 +/- .33
1 count = 0 magFe (starfind)
1 count = -25.87 mag (2MASS) = 1024 * 10^(-25.87/2.5) = 4.595e-8 Jy/count
multiply by .2/.0055 = 36.4
.273"/pix
surface brightness = 4.595e-8 * 206265**2 / .273**2 = 26.2e3 Jy / sr / count = .0262 MJy/sr/count
total counts for inner portion of nebula: 2.93e7
average counts = 3895 , 3895 * .0262 MJy/sr -> 102 MJy/sr
area = 1.317e-8 sr
total emission = 1.344e-7 MJy -> 4.865e-6 MJy = 486.5 mJy
outer nebula: total counts 1731540 npix: 74777 average: 23.2
tried a different way: star at 20:17:45.706 +38:02:17.23 has 14484 counts over 43 pixels
star at 20:17:43.052,+38:02:28.54 has 8150 counts over 22 pix, H-band mag 14.868 -> 1024 * 10^(-14.868/2.5) = 1.023e-3 Jy
-> 1.514e-7 Jy/count. Factor of 3 different, pretty close... could that be 1024, not 1.024 Jy? Yes.
star at 20:17:40.975 +38:02:26.20 has 6438 counts over 18 pix with Hmag 14.936 -> 1.086e-3 Jy -> 1.68e-7 Jy/count
say 1.60 +/- .1 * 10^-7 Jy/count * 36.4 for conversion from H to Fe filter
gives total emission of nebula 1731540 * 36.4 * 1.6e-7 = 10 Jy
central wavelength = 1.64um = 1.83e14 Hz
delta wavelength = .0055um. delta-nu = c/lambda^2 * delta-lambda = 6.13e11 Hz
area = (3.68e17 cm)^2 * pi = 4.25e35 cm^2
1 Jy * 4.25e35 cm^2 * 6.13e11 Hz = 2.61e21 erg/s / sr
Surface brightness recalculated with large Jy/ct: 1.60e-8 * (206265/.273)**2 * 3895 = 356 MJy/sr

For the outer nebula, two possible inner radius selections:
1. 45" - 14.5" -> 76710 pixels, 1814414 counts, average 23.65, surface brightness .22 MJy/sr
1. 45" - 19.35" -> 69752 pixels, 1006476 counts, average 14.4, surface brightness .13 MJy/sr


Recalculated things in April:
(these are calibrated to pcyg_feii1.64combine_rot0_240s.fits and phot.pcyg_feii1.64combine_rot0_240s.txt)
0.000483 +/- 0.000034 mJy/count in H-band
0.006485 +/- 0.000459 mJy/count/arcsec^2
i.e. 10000 counts corresponds to surf. brightness 65 mJy/arcsec^2
which in turn is 2.360 Jy/arcsec^2 in the [Fe II] narrow-band
Outer Nebula total: 11.8 Jy, average:.15 mJy / pix, 2.1 mJy / arcsec^2
Inner Nebula total: 190 Jy, average 25.3 mJy / pix, 339 mJy / arcsec^2