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Tracing the Extent of Narrow Line Emission in Type II QSOs

Tracing the Extent of Narrow Line Emission in Type II QSOs. Kevin Hainline & Ryan Hickox. Using SALT RSS longslit spectra of nearby Type II QSOs, we can measure the extent of the narrow-line region, and compare to the size of the galaxy stellar continuum. Greene et al. (2011).

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Tracing the Extent of Narrow Line Emission in Type II QSOs

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  1. Tracing the Extent of Narrow Line Emission in Type II QSOs Kevin Hainline & Ryan Hickox Using SALT RSS longslit spectra of nearby Type II QSOs, we can measure the extent of the narrow-line region, and compare to the size of the galaxy stellar continuum. Greene et al. (2011) SDSS J081125.8+073235.4 z = 0.35 [OIII] 5007 To estimate the spatial extent of our features, we deconvolve our observed lines with the seeing, and use a width that represents 10% of the maximum surface brightness. 2.0” Surface Brightness At z = 0.35, 2” corresponds to 9.9 kpc. (log R/pc = 3.99) Spatial Position (pixel)

  2. SDSS J084107.1+033441.3 Type II QSO z = 0.27 Top of slit 20” Galaxy rotation as measured through [OIII] 5007 narrow-line emission.

  3. SDSS J122217.9-00743.8 Type II QSO z = 0.17 Top of slit 20” A dual AGN, with [OIII] tracing the movement of both galaxies.

  4. I also wrote up my longslit reduction recipe here: http://www.astro.ucla.edu/~kevinhainline/salt_redux.html (or http://goo.gl/t4MPM) The site describes basic longslit reduction in a similar manner to what is described on the SALT wiki. Overall, while it would be good if there was some way of obtaining absolute flux calibration, there is a variety of science that we have been doing without an estimate of the absolute fluxes. Finally, I think SALT data could use extra information in the image headers, such as a calculation of the airmass and sidereal time for the observation.

  5. Rapid Supernova Identification and Follow-up With SALT A Target of Opportunity (ToO) campaign to classify nearby supernova candidates soon after they are discovered. Supernovae of interest may be monitored with additional follow-up spectra. The program is straightforward with rapid turn-around between initial observations and published identifications. PI: Robert Fesen CoI: Dan Milisavljevic CoI: Tim Pickering Paper submitted Paper forthcoming Papers forthcoming (DIBs changing!) Paper forthcoming

  6. This is paper one of many on the way. We are very grateful for help from: T. Pickering, S. Crawford, A. Kniazev, P. Kotze, Encarni Romero-Colmenero, Petri Vaisanen, Christian Hettlage, & A. Gulbis

  7. Rapid Supernova Identification and Follow-up With SALT • Questions: • Can method of triggering Target of Opportunity programs be improved? Currently need to email on case-by-case basis to request to unlock proposal and this isn’t always convenient. • Is there a way to rapidly access via web how many hours are left in a TOO program? • Do leftover TOO hours from one semester carry over into the next? • What is the official procedure when two TOO programs trigger on the same object?

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