Adaptive optics systems for HARMONI: a visible and near-infrared integral field spectrograph for the E-ELT

2010 ◽  
Author(s):  
Thierry Fusco ◽  
Niranjan Thatte ◽  
Serge Meimon ◽  
Matthias Tecza ◽  
Fraser Clarke ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Near Infrared ◽  
Integral Field Spectrograph ◽  
Integral Field

scholarly journals CS Cha B: A disc-obscured M-type star mimicking a polarised planetary companion

2020 ◽  
Vol 640 ◽  
pp. L12
Author(s):  
S. Y. Haffert ◽  
R. G. van Holstein ◽  
C. Ginski ◽  
J. Brinchmann ◽  
I. A. G. Snellen ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Near Infrared ◽  
Type Star ◽  
Atmospheric Models ◽  
Planetary Mass ◽  
Medium Resolution ◽  
Low Mass ◽  
Integral Field Spectrograph ◽  
Integral Field

Context. Direct imaging provides a steady flow of newly discovered giant planets and brown dwarf companions. These multi-object systems can provide information about the formation of low-mass companions in wide orbits and/or help us to speculate about possible migration scenarios. Accurate classification of companions is crucial for testing formation pathways. Aims. In this work we further characterise the recently discovered candidate for a planetary-mass companion CS Cha b and determine if it is still accreting. Methods. MUSE is a four-laser-adaptive-optics-assisted medium-resolution integral-field spectrograph in the optical part of the spectrum. We observed the CS Cha system to obtain the first spectrum of CS Cha b. The companion is characterised by modelling both the spectrum from 6300 Å to 9300 Å and the photometry using archival data from the visible to the near-infrared (NIR). Results. We find evidence of accretion and outflow signatures in Hα and OI emission. The atmospheric models with the highest likelihood indicate an effective temperature of 3450 ± 50 K with a log g of 3.6 ± 0.5 dex. Based on evolutionary models, we find that the majority of the object is obscured. We determine the mass of the faint companion with several methods to be between 0.07 M⊙ and 0.71 M⊙ with an accretion rate of Ṁ = 4 × 10−11±0.4 M⊙ yr−1. Conclusions. Our results show that CS Cha B is most likely a mid-M-type star that is obscured by a highly inclined disc, which has led to its previous classification using broadband NIR photometry as a planetary-mass companion. This shows that it is important and necessary to observe over a broad spectral range to constrain the nature of faint companions.

scholarly journals Evidence for an accreting massive black hole in He 2–10 from adaptive optics integral field spectroscopy

2020 ◽  
Vol 494 (2) ◽  
pp. 2004-2011 ◽  
Author(s):  
Rogemar A Riffel
Keyword(s):  
Black Hole ◽  
Adaptive Optics ◽  
Near Infrared ◽  
Dwarf Galaxy ◽  
Line Emission ◽  
Massive Black Hole ◽  
Star Forming ◽  
Star Forming Regions ◽  
Integral Field Spectrograph ◽  
Integral Field

ABSTRACT Henize 2–10 is a blue dwarf galaxy with intense star formation and one the most intriguing question about it is whether or not it hosts an accreting massive black hole. We use H and K-band integral field spectra of the inner 130 pc × 130 pc of He 2–10 to investigate the emission and kinematics of the gas at unprecedented spatial resolution. The observations were done using the Gemini Near-Infrared Integral Field Spectrograph (NIFS) operating with the ALTAIR adaptive optics module and the resulting spatial resolutions are 6.5 and 8.6 pc in the K and H bands, respectively. Most of the line emission is due to excitation of the gas by photoionization and shocks produced by the star forming regions. In addition, our data provide evidence of emission of gas excited by an active galactic nucleus located at the position of the radio and X-ray sources, as revealed by the analysis of the emission-line ratios. The emission lines from the ionized gas in the field present two kinematic components: one narrow with a velocity field suggesting a disc rotation and a broad component due to winds from the star forming regions. The molecular gas shows only the narrow component. The stellar velocity dispersion map presents an enhancement of about 7 km s−1 at the position of the black hole, consistent with a mass of $1.5^{+1.3}_{-1.3}\times 10^6$ M⊙.

scholarly journals Science with EPICS, the E-ELT planet finder

2010 ◽  
Vol 6 (S276) ◽  
pp. 343-348
Author(s):  
Raffaele Gratton ◽  
Markus Kasper ◽  
Christophe Vérinaud ◽  
Mariangela Bonavita ◽  
Hans M. Schmid
Keyword(s):  
Adaptive Optics ◽  
Near Infrared ◽  
Large Telescope ◽  
High Performing ◽  
System A ◽  
Reflected Light ◽  
Integral Field Spectrograph ◽  
Adaptive Optics System ◽  
Integral Field

AbstractEPICS is the proposed planet finder for the European Extremely Large Telescope. EPICS is a high contrast imager based on a high performing extreme adaptive optics system, a diffraction suppression module, and two scientific instruments: an Integral Field Spectrograph (IFS) for the near infrared (0.95-1.65 μm), and a differential polarization imager (E-POL). Both these instruments should allow imaging and characterization of planets shining in reflected light, possibly down to Earth-size. A few high interesting science cases are presented.

scholarly journals Spatially Resolved Spectroscopy to Confirm or Disprove Dual Active Galactic Nuclei

2013 ◽  
Vol 9 (S304) ◽  
pp. 371-374
Author(s):  
Rosalie C. McGurk ◽  
Claire E. Max ◽  
Anne Medling ◽  
Gregory A. Shields
Keyword(s):  
Emission Line ◽  
Active Galactic Nuclei ◽  
Adaptive Optics ◽  
Near Infrared ◽  
Galactic Nuclei ◽  
Spatially Resolved ◽  
Spatially Resolved Spectroscopy ◽  
Integral Field Spectrograph ◽  
Guide Star ◽  
Integral Field

AbstractWhen galaxies merge, gas accretes onto both central supermassive black holes. Thus, one expects to see dual active galactic nuclei (AGNs) in a fraction of galaxy mergers. Candidates for galaxies containing dual AGNs have been identified by the presence of double-peaked narrow [O III] emission lines and by high spatial resolution images of close galaxy pairs. 30% of double-peaked narrow [OIII] emission line SDSS AGNs have two spatial components within a 3″ radius. However, spatially resolved spectroscopy is needed to confirm these galaxy pairs as systems with double AGNs. With the Keck 2 Laser Guide Star Adaptive Optics system and the OSIRIS near-infrared integral field spectrograph, we obtained spatially resolved spectra for SDSS J095207.62+255257.2, confirming that it contains a Type 1 and a Type 2 AGN separated by 4.8 kpc (=1.0″). We performed similar integral field and long-slit spectroscopy observations of more spatially separated candidate dual AGNs and will report on the varied results. By assessing what fraction of radio-quiet double-peaked emission line SDSS AGNs are true dual AGNs, we can better constrain the statistics of dual AGNs and characterize physical conditions throughout these interacting AGNs.

scholarly journals Near-Infrared Spectroscopy of the Surface of Mars Derived from TIGER Spectro-Imaging Data

1995 ◽  
Vol 149 ◽  
pp. 298-299
Author(s):  
P. Martin ◽  
P.C. Pinet ◽  
R. Bacon ◽  
A. Rousset
Keyword(s):  
Infrared Spectroscopy ◽  
Spatial Resolution ◽  
Near Infrared Spectroscopy ◽  
Near Infrared ◽  
Western Hemisphere ◽  
Imaging Data ◽  
Integral Field Spectrograph ◽  
Integral Field ◽  
Spectro Imaging

AbstractHigh spectral and spatial resolution telescopic observations of the western hemisphere of Mars, using the integral field spectrograph TIGER at 0.8-1.1 µm, are described.

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