Astronomical Spectroscopy - Physics - University of Cincinnati

More documents

Recommendations

Info

$1 Ch. 22 â Reflection and Refraction of Light 22.1 The ... - Physics$

– 74 – Fig. 19.— Spatial cut across Hydra data. The spectra of many stars have been obtained in a single exposure, but which star is which
– 75 – 500 stars. Figure 20 shows the Tonry & Davis (1979) r parameter (a measure of how well the cross-correlation worked) versus the radial velocity of each star. There are clearly two distributions, one centered around a velocity of zero (expected for foreground stars) and one centered around 160 km s −1 , the radial velocity of the SMC. All together 176 certain and 16 possible SMC supergiants were found, and their numbers in the H-R diagram were used to show that the current generation of stellar evolutionary models greatly over estimate the duration of this evolutionary phase (Neugent et al. 2010). Since a similar finding had been made in the higher metallicity galaxy M31 (using radial velocities from Hectospec; Drout et al. 2009) the SMC study established that uncertainties in the mass-loss rates on the mainsequence must not be to blame. The OI λ7774 line proved to be a useful luminosity indicator even at relatively low metallicities. 150 100 50 -100 0 100 200 300 Fig. 20.— The radial velocities of SMC F/G supergiant candidates. The Tonry & Davis (1979) r parameter is plotted against the radial velocity of approximately 500 stars observed with Hydra at the CTIO 4-m telescope. The stars with radial velocities
Page 1 and 2:
Astronomical Spectroscopy Philip Ma
Page 3 and 4:
- 3 - Similarly the emphasis here w
Page 5 and 6:
- 5 - could see 8000Å light from f
Page 7 and 8:
- 7 - ratio of the focal lengths of
Page 9 and 10:
- 9 - Fig. 2.— The overlap of var
Page 11 and 12:
- 11 - 2.1.2. Choosing a grating Wh
Page 13 and 14:
- 13 - 4-Meter Telescope - RC Spect
Page 15 and 16:
- 15 - gratings blazed at the red.
Page 17 and 18:
- 17 - each order (Equation 9). Thi
Page 19 and 20:
- 19 - wants can be a real challeng
Page 21 and 22:
- 21 - Fig. 7.— Multi-object mask
Page 23 and 24: - 23 - Fig. 8.— Optical layout of
Page 25 and 26: - 25 - Fig. 9.— View of the focal
Page 27 and 28: - 27 - Fig. 10.— Optical design o
Page 29 and 30: - 29 - When built twenty years ago,
Page 31 and 32: - 31 - corrected” image cube is c
Page 33 and 34: - 33 - • The data frames themselv
Page 35 and 36: - 35 - Fig. 11.— Three examples o
Page 37 and 38: - 37 - bumps and wiggles are presen
Page 39 and 40: - 39 - Fig. 13.— The spatial prof
Page 41 and 42: - 41 - one might want to do this on
Page 43 and 44: - 43 - The steps involved in this r
Page 45 and 46: - 45 - be obtained for each grating
Page 47 and 48: - 47 - the flat-field division. Alt
Page 49 and 50: - 49 - night. More about this is di
Page 51 and 52: - 51 - can be answered given a comp
Page 53 and 54: - 53 - that it degraded the signal-
Page 55 and 56: - 55 - 3.2.6. Long-Slit Flat-Fieldi
Page 57 and 58: - 57 - over the “perfect” flat-
Page 59 and 60: - 59 - 3.2.7. Radial velocities and
Page 61 and 62: - 61 - A good general line list (id
Page 63 and 64: - 63 - the only overlap would be wi
Page 65 and 66: - 65 - a far better job at matching
Page 67 and 68: - 67 - dispersion. Going to the par
Page 69 and 70: - 69 - red (including at least 7770
Page 71 and 72: - 71 - Exposures of the dome flat q
Page 73: - 73 - A bright star was seen just
Page 77 and 78: - 77 - So, attempt to select a tell
Page 79 and 80: - 79 - Fig. 21.— Output from the
Page 81 and 82: - 81 - Wrap-Up and Acknowledgements
Page 83 and 84: - 83 - Massey, P., DeVeny, J., Jann
show all

Astronomical Spectroscopy - Physics - University of Cincinnati

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?