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The Las Campanas Prism Survey

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Wide Field Integral Spectroscopy with PrISM Jeff Rich GalPath Barry Madore, Mark Seibert, Vicky Scowcroft, Laura Sturch Massive IFU Surveys: a data cube for every galaxy -Surveys collecting Integral Field Spectra (IFS) for >10,000 galaxies -ATLAS3D, CALIFA, SAMI, MaNGA, smaller surveys -IFS data allows us to examine transformative processes in detail The WiFeS GOALS Survey: IFS of 40 Merging galaxies Rich et al. 2015 R-band Digitized Sky Survey images WiFeS Field of View overlaid The WiFeS GOALS Survey 370-700 nm, R~7000 25”x38” FOV 40 individual galaxies, from beginning to end of merger sequence Redshift of 0.009 - 0.049 -200-900 parsecs/pix (650-3000 lyr/pix) Measuring ISM Properties -Low spatial resolution, relatively high spectral resolution -Resolve individual velocity components in single LOS, compare with line ratios -Separate HII region, AGN, Shocks, measure O/H, kinematics Rich et al. 2011, ApJ, 734, 87 Measuring ISM Properties Nuclear vs. Resolved Spectroscopy IFS data reveal that ISM is ionized by radiative shocks =>Single fiber/slit data can misidentify AGN [O III]/Hb x NGC 3256 Rich et al. 2011, 2014 WiFeS GOALS Survey Using Shocks to Trace Gas Flows Caused by Merger Process Isolated (3) Widely Separated ‘a’ (4) Closely Interacting ‘b’ (9) Coalesced ‘cde’ (3) Using Shocks to Trace Gas Flows Caused by Merger Process -Young stars dominate emission Young Stars before merger, Shocks increasingly contribute to emission as mergers Shocks progress -Shocks trace increasing inflows Turbulent Star Formation and outflows during merger -Presence of Shocks can affect typical measurements made with emission lines (O/H, SFR, etc.) Using Metallicity to Trace Gas Flows Spectra from data cubes can be ESO 138-G27 used to measure metallicity via strong-emission line methods Undisturbed spiral galaxies show a gradient in [O/H], decreasing from the center to the outskirts Gas flows in merger are predicted to disrupt this gradient [O/H] Using Metallicity to Trace Gas Flows Before Merger: Steep Metallicity Gradient ESO 138-G27 Oxygen [O/H] Oxygen Radial Distance Rich et al. 2012 Using Oxygen to Trace Gas Flows During/After Merger: No Metallicity Gradient IC 1623 Oxygen [O/H] Oxygen Radial Distance Rich et al. 2012 Resolution v. O/H Gradient -Spatial resolution of data can impact measurements -Poor resolution results in underprediction of metallicity gradient Yuan, Rich & Kewley 2013 Resolution v. Dynamics Kinemetry derived from IFS can be used to identify merger activity (Krajnovic+06, Shapiro+08, Bellocchi+12) Shapiro et al. 2008 Rich et al. 2011, ApJ, 734, 87 Resolution v. Dynamics -Spatial resolution can affect Merger/Disk kinematic classifications -Kinematics from low-res IFU data cannot constrain merger fraction of z~1-3 galaxies Hung et al. 2015 High(er) Spatial Resolution? Nearby galaxies yield intrinsically high(er) resolution ...but require significantly more time to observe NGC NGC 1365 3256 Progressive Integrated Stepping Method (PrISM) Integral Wide-Field Narrow Band Imaging Stacked Integral Progressive Integral Spectrsocopy (e.g Fabry-Pérot) Field Units Step Method (PrISM) y (arc-minutes) wavelength x (arc-minutes) Spatially Resolved Galaxy IFS: Simple Execution: star formation modern telescope control systems star formation histories desktop computing power chemical evolution cheap disk storage separated by morphological components ~ $0 SLS/PrISM Concerns INEFFICIENT true for small objects true for faint objects use for large bright objects VARIABLE SKY true always ultra-long slit allows for simultaneous sky for each exposure if diameter < slit. PrISM Specifications @LCO du Pont Table 1. PrISM Specifications Field of view (slit) 18’ 1.65” (0.5 arcminute2) ⇥ 1 Spectral resolution R=800 (375 km s− FWHM) Spaxel size 1.65” 0.484” (native) / 1.65” 1.65” (binned) ⇥ ⇥ Spatial resolution 2 – 177 pc (48 pc median) Spectral range 3650 – 9000 A˚ a 17 1 2 1 Flux limit (5000A)˚ 4 10− erg s− cm− A˚ − per resolution element ⇥ 33.4 µJy per resolution element µ = 21.1 AB mag / arcsec2 S/N=3, 600 sec., 1.652 arcsec spaxel Telescope 2.5m f/7.5 du Pont telescope, Las Campanas, Chile Camera/Detector Wide Field reimaging CCD (WFCCD) 25 arcminute diameter field WF4K 4064 4064 CCD ⇥ Note. — (a) Spatial binning will provide high S/N measurements far below this limit. ~72 arcsec aperture Typhoon vs SDSS Nucleus of UGC1382 ~7 sqr−arsec aper. /A] 250 2 200 SDSS 2700 sec. Test Case: Typhoon 600 sec. 150 Typhoon S/N erg/s/cm 17 100 − 50 0 recreating SDSS flux [10 4000 5000 6000 7000 8000 wavelength [A] /A] 200 2 150 100 erg/s/cm 17 − PrISM 600sec 50 0 flux [10 3800 4000 4200 4400 4600 SDSS 2700sec wavelength [A] /A] 250 2 200 150 erg/s/cm 17 − nucleus of UGC1382 100 50 flux [10 4600 4800 5000 5200 5400 5600 distance=80 Mpc wavelength [A] /A] 250 2 200 erg/s/cm 22 steps 17 − 150 100 0.6’ x 8.9’ flux [10 5600 5800 6000 6200 6400 6600 wavelength [A] /A] 250 2 200 erg/s/cm 17 1.65”x1.65” − 150 100 flux [10 6600 6800 7000 7200 7400 7600 binned pixel scale wavelength [A] /A] 250 2 200 erg/s/cm 17 − 150 100 flux [10 7600 7800 8000 8200 8400 wavelength [A] M83 / NGC5236 Raw Data 5 Nights 179 Spectra 5’ x 18’ Reduction is like long slit data but with 2D distortion corrections over entire FOV BVR+Hα M83 / NGC5236 5 Nights 179 Spectra 5’ x 18’ Reduction is like long slit data but with 2D distortion corrections over entire FOV ~9x108 voxels @native res. ~3x108 voxels @binned res. relative flux 12 arc-minutes 4000 4500 5000 5500 6000 6500 7000 wavelength [Å] 5 arc-minutes SINGGS NB Imaging PrISM Extraction λ=6568Å Δ 30Å λ=6568Å Δ 30Å 10 10 5 5 0 0 -5 -5 Meurer et al. 2006 (binned at 1.65”) 2006 (binnedat al. et Meurer -10 -10 -2 0 2 kpc -2 0 2 kpc -0.6 0.3 1.2 2.1 3.0 log erg/s/cm 2/Å/1e-17 H [OIII] H [NII] [SII] 6717Å [SII] 6731Å 0 0 0 0 0 0 412 pc / pixel 412 pc / pixel 412 pc / pixel 412 pc / pixel 412 pc / pixel 412 pc / pixel 02kpc 02kpc 02kpc 02kpc 02kpc 02kpc 4 0.11.2 2..2 12 4 12 4 1.12.0 2. 1.12.0 log erg/s/cm 2 log erg/s/cm 2 log erg/s/cm 2 log erg/s/cm 2 log erg/s/cm 2 log erg/s/cm 2 Velocity Vel. Dispersion [NII]/H [OIII]/H Metallicity (O3N2) Gas Density 0 0 0 0 0 0 412 pc / pixel 412 pc / pixel 412 pc / pixel 412 pc / pixel 412 pc / pixel 412 pc / pixel 02kpc 02kpc 02kpc 02kpc 02kpc 02kpc 0 2..0 .0 4. 0.0 .0 0. 1.01 2.02 km/s / Å log flux ratio log flux ratio 12 + log(O/H) log Ne 40,000 spectra 41x41 pc resolution PrISM M83 Resolved BPT 8.00 8.00 1.0 7.75 7.75 7.50 7.50 7.25 7.25 7.00 7.00 0.5 6.75 6.75 6.50 6.50 ionization par. ionization par. ] b 0.0 log[OIII/H -0.5 -1.0 12+log(O/H) 12+log(O/H) 9.17 9.17 8.99 8.99 8.69 8.69 -1.5 -1.0 -0.5 0.0 0.5 1.0 -1.0 -0.5 0.0 0.5 log[NII/Ha] log[SII/Ha] J. Rich (in progress) Las Campanas Observatory PrISM Survey (AKA Typhoon) Table 3. PrISM Survey Targets Target Type Major Axis Minor Axis BTotal Distance Resolution No. % 1 arcmin arcmin mag Mpc pc spaxel− Steps Observed WLM IB 10.5 3.5 11.0 0.92 7.4 129 NGC 24 Sc 6.2 2.4 12.1 8.13 64.9 87 NGC 45 SABd 6.2 4.5 11.4 7.07 56.5 162 NGC 55 SBm 30.2 3.1 8.5 2.17 17.3 112 NGC 59 E-SO 2.4 1.3 13.1 5.30 42.3 45 IC 1574 IB 1.8 0.7 14.5 4.92 39.3 25 Sample NGC 247 SABc 19.5 5.5 9.7 3.65 29.2 199 NGC 253 SABc 26.9 4.6 7.9 3.94 31.5 166 38 NGC 289 SBbc 5.1 3.6 22.45 107.0 Galaxies large enough to take advantage of NGC 300 Scd 19.5 12.9 8.8 2.00 16.0 468 80 IC 1613 I 12.9 12.0 10.1 0.65 5.2 437 NG C0625 SBm 6.6 2.1 11.6 4.07 32.5 75 scanning method and near enough to study at ESO 245-G005 IB 3.2 3.1 12.8 4.43 35.4 112 M 77 Sb 6.2 5.6 9.7 12.65 100.9 204 31 ESO154-G023 SBm 4.8 1.1 12.8 5.76 46.0 40 spatial scales not reached by other surveys. NGC 1291 S0-a 11.2 10.0 9.4 9.37 74.8 363 NGC 1313 SBcd 11.0 9.1 9.6 4.15 33.2 331 12 NGC 1311 SBm 3.7 0.9 13.4 5.45 43.5 33 NGC 1316 S0 13.5 7.8 9.4 20.17 160.5 282 24 NGC 1365 Sb 12.0 6.2 10.4 18.15 144.5 224 75 NGC 1399 E 8.5 7.8 10.4 18.28 145.6 282 25 Local Volume Legacy Survey NGC 1404 E 5.0 4.4 10.9 19.09 152.0 158 34 NGC 1487 Scd 2.7 2.1 12.3 9.08 72.5 75 Galaxies within 11 Mpc (Dale et al.
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  • ASTRONOMY and ASTROPHYSICS Ultraviolet Spectral Properties of Magellanic and Non-Magellanic Irregulars, H II and Starburst Galaxies?

    ASTRONOMY and ASTROPHYSICS Ultraviolet Spectral Properties of Magellanic and Non-Magellanic Irregulars, H II and Starburst Galaxies?

    Astron. Astrophys. 343, 100–110 (1999) ASTRONOMY AND ASTROPHYSICS Ultraviolet spectral properties of magellanic and non-magellanic irregulars, H II and starburst galaxies? C. Bonatto1, E. Bica1, M.G. Pastoriza1, and D. Alloin2;3 1 Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501–970, RS, Brazil 2 SAp CE-Saclay, Orme des Merisiers Batˆ 709, F-91191 Gif-Sur-Yvette Cedex, France Received 5 October 1998 / Accepted 9 December 1998 Abstract. This paper presents the results of a stellar popula- we dedicate the present work to galaxy types with enhanced 1 1 tion analysis performed on nearby (VR 5 000 km s− ) star- star formation in the nearby Universe (VR 5 000 kms− ). We forming galaxies, comprising magellanic≤ and non-magellanic include low and moderate luminosity irregular≤ galaxies (magel- irregulars, H ii and starburst galaxies observed with the IUE lanic and non-magellanic irregulars, and H ii galaxies) and high- satellite. Before any comparison of galaxy spectra, we have luminosity ones (mergers, disrupting, etc.). The same method formed subsets according to absolute magnitude and morpho- used in the analyses of star clusters, early-type and spiral gala- logical classification. Subsequently, we have coadded the spec- xies (Bonatto et al. 1995, 1996 and 1998, hereafter referred to tra within each subset into groups of similar spectral proper- as Papers I, II and III, respectively), i.e. that of grouping objects ties in the UV. As a consequence, high signal-to-noise ratio with similar spectra into templates of high signal-to-noise (S/N) templates have been obtained, and information on spectral fea- ratio, is now applied to the sample of irregular and/or peculiar tures can now be extracted and analysed.