Active Galactic Nuclei research with SOAR: present and upcoming capabilities

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1 Active Galactic Nuclei research with SOAR: present and upcoming capabilities SOAR 2020 WORKSHOP CBPF Rio de Janeiro March / 2017 Courtesy: Gabriel Maturana/NOAO/AURA/NSF Alberto Rodríguez Ardila LNA/MCTIC

2 OUTLINE Current instrumentation at SOAR Upcoming AGN The instrumentation introduction Broad Line Region - Goodman Detection SIFS of outflows Spectroscopy ARCOiRIS spectroscopy

3 CURRENT INSTRUMENTATION GHT Spectrograph SAM + FP

4 UPCOMING INSTRUMENTATION ARCoIRIS is a cross-dispersed, singleobject, longslit, infrared imaging spectrograph, containing no moving parts. Features a fixed slit of 1.1 x 28. Spectra cover a simultaneous wavelength range of 0.80 to 2.47 μm, at R ~ 3500 (z'yjhk photometric range). SIFS - IFU with 1300 fibers Microlenses matrix of 26 x 50 Two physical scales: 0,15"/pixel, FoV 3,9x7,5" 0,3"/pixel, FoV 7,8x15" IFU for sky VPH gratings with R ~ 1K - 5K

5 Unified model of Active Galactic Nuclei

6 Unified model of Active Galactic Nuclei

7 Unified model of Active Galactic Nuclei

8 THE MBH σ* RELATIONSHIP Credit: Gültekin et al. (2009) Suggests some kind of evolutionary link between the growth of galaxies and the growth of SMBH. Ultimate goal is to study the AGN feedback by means of ionized gas outflows. Reconigzed as a crucial ingredient in the MBH - * relationship (e.g. Gebhardt et al. 2000).

9 TWO-WAY COMMUNICATION How are supermassive black holes fed? How is their growth regulated? local feedback How do supermassive black holes affect their surroundings on galactic scales? global feedback

10 BROAD LINE REGION STUDIES Spectra of quasars show absorption lines information of the intermediate gas. Formed by gas associated with the quasar. Diagnostic tools for its surroundings Most lines are blueshifted gas is flowing out of the center. The study of these absorptions increase our understanding of outflow and quasar feedback. Detached BALs in the quasar PG (Hamann 1998). The BALs are labeled just above the spectrum. The wavelengths of prominent broad emission lines are marked across the top. The Flux has units ergs s-1 cm-2 Å-1. Intrinsic absorption in the quasar PG (Hamann et al 1997). A system of associated NALs is labeled above the spectrum, with open brackets showing the doublet separations. A mini-bal due to CIV blueshifted by ~51,000 km/s is labeled below. The Flux has units10-15 ergs s-1 cm-2 Å-1.

11 (Benn et al. 2005) Goodman red camera, free of fringing effects to the red end allows this type of studies. Spectrum taken with the 4.2 m WHT; 2 x 1800 s exposure. The broad trough centred at 6230Å is due to CIV absorption by gas streaming out from the quasar at between 21,000 and 29,000 km s-1 (i.e.~0.1c). The physics of the acceleration and confinement of the gas in BAL outflows is unknown.

12 The FeII problem One of the most puzzling aspects of the BLR of AGNs including QSOs at z 6 is the FeII emission (Wills et al. 1985; Baldwin et al. 2004). Numerous multiplets form a pseudo-continuum from the UV to the NIR due to the blending of approximately 105 lines. It is one of the most important contributors to the cooling of the BLR!! Important probe of AGN physics. The strength of the Fe II λ4570 emission relative to [OIII] λ5007 is a dominant variable in the first principal component (PC1 or Eigenvector 1, Boroson & Green 1992). Generally believed to be linked to certain fundamental parameters of the accretion process: L/LEdd or L/M (Sulentic et al. 2000; Boroson 2002). Its study leads to understand the properties of the emission line region that is closest to the central source. More on this topic see Murilo Marinello' s talk

13 SIFS ENGINEERING TESTS SIFS has been tested on-sky on engineering nights and Brazilian DDT. 50 x 26 fibers, 0.3 /fiber. FOV of 15 x 7 Detector is an E2V 4K x 4K CCD. Setup tested includes a 700 l/mm grating; provides a ~2800 Å coverage in wavelength; Δλ = Å/pix; R ~ 2500 at 5500 Å. NGC 3081, a Sy2 galaxy was observed in January 17, exposures of 1200 s each were taken. Average seeing during observations ~0.8 Very preliminary results will be shown here.

14 NGC 3081 OBSERVED WITH SIFS Nuclear spectrum,~ 0.9 centred at the AGN.

15 [OI]+ [FeX]

16 NGC 3081 OBSERVED WITH SIFS A A ~ 2.1 South of the nucleus

17 SOAR INTEGRAL FIELD SPECTROGRAPH SIFS: 3D SPECTROSCOPY

18 THE SOAR INTEGRAL FIELD SPECTROGRAPH - SIFS a) Detect and study the statistical, geometric and physical properties of Low Luminosity AGN (LLAGN). b) Circumnuclear emission line properties. Nature, ionization mechanism as well as the kinematics of the line emitting gas. c) how mass is transferred from kiloparsec scales down to nuclear scales? d) Outflows mapped by means of high-ionization forbidden lines.

19 [SVIII] ARCOiRIS: A NEW CAPABILITY IN THE NIR Paδ HeII [SII] [FeXIII]

20 ARCOiRIS: NEW CAPABILITIES IN THE NIR

21 ARCOiRIS: NEW CAPABILITIES IN THE NIR [SiIX] [SiVI] Brδ [CaVIII]

22 ARCOiRIS SCIENCE DRIVERS FOR AGN Evidence of AGN winds is growing, with the discovery of multiple observational examples in all gas phases (e.g. Feruglio et al. 2015; Maiolino et al. 2012; Fabian 2012; Harrison et al. 2012; Spoon et al. 2013; Rupke & Veilleux 2015; Brusa et al. 2015; Morganti et al. 2016), ARCOiRIS is a prime instrument for the detection of such powerful outflows in z = 2 3 AGNs using the [OII] 5007 line as diagnostics. FeII emission in the NIR; High-z sources for optical FeII. In combination with Goodman, possibility of nearly-simultaneous OIR spectroscopy, from 4500 Å up to Å For nearby sources, the wealth of emission lines added to the optical ones are tight constrains for photoionization models. Understand the physical mechanisms and conditions of the ionized gas (SIFS).

23 Serendipitously discovering of AGNs Z=1.887 Z=1.257 Z= Z= λ (Å) Oliveira et al λ (Å)

24 TAKE-AWAY MESSAGE AGN studies strongly benefits from SOAR. Main science drivers include: - Study of energetic outflows associated to the central engine. - How gas is transported from galactic scales down to the BH. - BALs and NALs in High-z sources. - FeII emission in the UV/Opt/NIR. - Morphology and physical properties of the AGN emission line regions. - Facility to DES & LSST follow-up, covering a large range in z.