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What it is The one we are building The kind of science one can do with it

A very short intro to the integral field spectroscopy (IFS) and the kind of cool stuff one can do with it. What it is The one we are building The kind of science one can do with it Work I’ve done and am going to do. Traditionally, use long slits to get spectroscopy.

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What it is The one we are building The kind of science one can do with it

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  1. A very short intro to the integral field spectroscopy (IFS) and the kind of cool stuff one can do with it

  2. What it is • The one we are building • The kind of science one can do with it • Work I’ve done and am going to do

  3. Traditionally, use long slits to get spectroscopy. - Differential atmospheric refraction (DAR) light is diffracted by the atmosphere; need to record separate exposures for each position or use A ADC(Amanda)

  4. Also, if we have something like this: Long slit doesn’t work well on diffused objects.

  5. With IFS, one can: star SAO 17796 See Arribas.S. et. 1999 for how to do the Differential atmospheric refraction on IFS

  6. The design of IFS The one Gerald is building (most popular): Katie:

  7. Multi-object spectroscopy (MOS) uses several bundles to obtain spectra of multiple, separated objects

  8. Spectrograph input

  9. Imaging fov 7.2 arcmin diameter Spectrographic field of view 3 x 5 arcmin The wavelength range of the GS is 310-750 nm If use Ha, this is up to z = 0.13 If use Oiii (5007), this is up to z = 0.5

  10. What can one do with it? One of the many things: 2D kinematics! – what I reduced from a similar instrument called Sparsepak 82 fibers Bigger fov and operates at lower redshifts The outside ones are sky fibers It’s on Kitt Peak National Observatory

  11. The DensePak

  12. Current sites having Integral Field Spectroscopy http://ifs.wikidot.com/instruments http://maps.google.com/maps/ms?msa=0&msid=112598494528527909135.000474e4434a677fe621f&ct=onebox&cd=20&cad=docsearch,cid:16013500208979677175&geocode=FeB8LgEdXa-79g

  13. Now some pretty images

  14. z_virgocentric = 0.00681471 z_desired = 0.18950001 z_actual = 0.18950001

  15. UGC 6206 z_virgocentric = 0.00681471 z_desired = 0.055500003 z_actual = 0.055500003

  16. UGC 9869 (rotated to somehow fit) z_virgocentric = 0.00681471 z_desired = 0.042500002 z_actual = 0.042500002

  17. From this wonderful wikipedia website dedicated for IFS - ifs.wikidot.com: • Pre-main sequence objects • Proto-stellar discs, jets, Herbig Haro objects, collimation, mass loss, mass accretion, pre-solar nebula • Resolved stellar populations • Local group and nearby galaxies, crowded fields, nuclear and bulge regions, most luminous stars, B and A supergiants, supernovae, Luminous Blue Variables, planetary nebulae, novae and cataclysmic variables, HII regions • Normal Galaxies • Stellar and gas dynamics, supermassive black holes, galaxy nuclei, elliptical galaxies, spirals/bars • Active Galaxies • Gas dynamics, stellar populations, nuclear activity/starburst, fuelling of the active nucleus, (extended) narrow emission-line regions • Groups and cluster of galaxies • Galaxy formation, galaxy evolution, tidal interaction and merging, star formation history • High redshift galaxies • Galaxy evolution, galaxy dynamics, galaxy formation, star formation history, cosmology • Gravitational lensing • Gravitational lens models, QSO unresolved structure, dark matter in lens galaxies, extinction laws in galaxies

  18. Resolved stellar populations (inc. HII regions & Planetary Nebulae) • Tsamis et al., 2008, MNRAS, 386, 22 (ADS) • Blum & McGregor 2008, AJ, 135, 1708 (ADS) • Davidge et al., 2008, ApJ, 677, 238 (ADS) • Pre-main sequence objects • Lavalley et al., 1997, A&A, 327, 671 (ADS) • Beck et al., 2004, AJ, 127, 408 (ADS) • Vasconcelos et al., 2005, AJ, 130, 1707 (ADS) • McGregor et al., 2007, Ap&SS, 311, 223 (ADS) • Beck et al., 2007, AJ, 133, 1221 (ADS) • Takami et al., 2007, ApJL, 670, 33 (ADS) • Perrin et al., 2007, ApJ, 670, 499 (ADS) • Beck et al., 2008, ApJ, 676, 472 (ADS) • Lopez, R. et al., 2008, MNRAS, 384, 464 (ADS) • Gustafsson et al., 2008, A&A, 488, 235 (ADS) • Giannini et al., 2009 A&A, 481, 123 (ADS) • Lopez, R. et al., 2008, MNRAS, 391, 1107 (ADS) • Aspin et al., 2009 AJ, 137, 431 (ADS) • Galaxies • Homeier & Gallagher, 1999, ApJ, 522, 199 (ADS) • Emsellem et al., 2004, MNRAS, 352, 721 (ADS) (1st science paper from the SAURON project) • Sugai et al., 2004, ApJ, 615, L89(ADS) • Garcia-Lorenzo et al., 2005, ApJ, 621, 146 (ADS) • Sugai et al., 2005, ApJ, 629, 131(ADS) • Barbosa et al., 2006, MNRAS, 371, 170 (ADS) • Christensen et al., 2006, A&A, 452, 869 (ADS) • Förster Schreiber et al., 2006, ApJ, 645, 1062 (ADS) (1st paper from the SINS Survey team) • Swinbank et al., 2007, MNRAS, 376, 479 (ADS) • Sugai et al., 2007, ApJ, 660, 1016(ADS) • Westmoquette et al., 2007, MNRAS, 381, 894 (ADS) • Krajnović et al., 2008, MNRAS, 390, 93 (ADS) • Genzel et al., 2008, ApJ, 687, 59 (ADS) (SINS survey - major follow-up paper) • Seth et al., 2008, ApJ, 687, 997 (ADS) • Riffel et al., 2008, MNRAS, 385, 1129 (ADS) • Böker et al., 2008, AJ, 135, 479 (ADS) • Riffel et al., 2008, MNRAS, 385, 1129 (ADS) • Goto et al., 2008, MNRAS, 386, 1355(ADS) • Vanzi et al., 2008, A&A, 486, 393 (ADS) • Kehrig et al. 2008, A&A, 477, 813 (ADS) • Garcia-Lorenzo et al., 2008, ApJ, 677,201 (ADS) • Westmoquette et al., 2009, ApJ, 696, 192 (ADS) • Storchi-Bergmann et al., 2009, MNRAS, 394, 1148 (ADS) • James et al., 2009, MNRAS, 2009, 398, 2 (ADS) • Lagos et al., 2009, AJ, 137, 5068 (ADS) • Bordalo et al. 2009, ApJ, 696, 1668 (ADS) • Matsubayashi et al. 2009, ApJ, 701, 1636 (ADS) • Krajnovic et al., 2009 (astroph) (Innovative uses of the LGS system with Gemini NIFS) VLT/VIMOS on the European Southern Observatory in Chile Wavelength 4000 - 11500 A 2D KINEMATICS AND PHYSICAL PROPERTIES OF Z~3 STAR-FORMING GALAXIES M. Lemoine-Busserolle 2009

  19. For VVDS-8666 used the GALFIT software to deduce the morphological parameters such as the center, the position angle, and the axial ratio. PA = 41 East of North and an inclination of i = 51

  20. Used disk model kinematic centre (x0,y0), the position angle (PA), the inclination (i), the velocity offset (Vs) of the centre relative to the integrated spectrum, the velocity curve Vc(r), and the thickness of the rotating disk.

  21. Star formation rates for VVDS-5183, following Kennicutt (1998a) scaled to a Chabrier (2003) IMF: SFR (Myrsun) = 0.83x10^-28L1500 (ergs/sHz)

  22. Back to our IFU Under progress: Allows all 12 motors to be controlled from LabVIEW interface

  23. In the future… Putting it together Jo will install and test it next spring I will come up with a commission plan to test: Flexure of xy actuators / Position repeatability The effect of the fiber flexures. Photometric throughput in terms of wavelength Cross-talk between fibers

  24. http://www.aanda.org/articles/aa/full/2007/27/aa6359-06/img47.gifhttp://www.aanda.org/articles/aa/full/2007/27/aa6359-06/img47.gif http://www.astro.lightarts.net/Nebulae/OrionII.jpg http://www.physics.unc.edu/~fheitsch/images/linemaps.jpg Arribas,S.1999Differential atmospheric refraction in integral-field spectroscopy: Effects and correction. Atmospheric refraction in IFS http://ifs.wikidot.com/local--files/what-is-ifs/ifu_designs.jpg Deployable multi-IFU for Goodman Spectrograph – Gerald Cecil http://maps.google.com/maps/ms?msa=0&msid=112598494528527909135.000474e4434a677fe621f&ct=onebox&cd=20&cad=docsearch,cid:16013500208979677175&geocode=FeB8LgEdXa-79g http://nedwww.ipac.caltech.edu/ M. Lemoine-Busserolle (2009) 2D KINEMATICS AND PHYSICAL PROPERTIES OF z 3 STAR-FORMING GALAXIES

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