scholarly journals The role of the JWST near-infrared spectrograph NIRSpec in understanding the assembly and evolution of galaxies

2019 ◽  
Vol 15 (S352) ◽  
pp. 336-336
Author(s):  
Catarina Alves de Oliveira
Keyword(s):  
Wavelength Range ◽  
Near Infrared ◽  
Target Selection ◽  
Field Of View ◽  
High Contrast ◽  
Evolution Of Galaxies ◽  
James Webb Space Telescope ◽  
Field Unit ◽  
Integral Field

AbstractThe near-infrared spectrograph NIRSpec is one of four instruments aboard the James Webb Space Telescope (JWST). It offers seven dispersers covering the wavelength range from 0.6 to 5.3 micron with resolutions from R ∼ 100 to R ∼ 2700. Using an array of micro-shutters for target selection, the multi-object spectroscopy mode of NIRSpec will be capable of obtaining spectra from a few tens to more than 200 objects simultaneously. It also features an integral field unit with a 3 by 3 arcseconds field of view, and various slits for high contrast spectroscopy of individual objects. We will provide an overview of the capabilities and performances of these three observing modes highlighting how NIRSpec will contribute to the quest to further understand the assembly and evolution of galaxies from the end of re-ionisation epoch to the present day.

scholarly journals ESO Spectroscopic Facility

2017 ◽  
Vol 13 (S334) ◽  
pp. 242-247
Author(s):  
Luca Pasquini ◽  
B. Delabre ◽  
R. S. Ellis ◽  
J. Marrero ◽  
L. Cavaller ◽  
...  
Keyword(s):  
High Resolution ◽  
Wavelength Range ◽  
Focal Plane ◽  
Working Group ◽  
Field Of View ◽  
High Resolution Spectroscopy ◽  
Wide Field ◽  
Low Resolution ◽  
Field Unit ◽  
Integral Field

AbstractWe present the concept of a novel facility dedicated to massively-multiplexed spectroscopy. The telescope has a very wide field Cassegrain focus optimised for fibre feeding. With a Field of View (FoV) of 2.5 degrees diameter and a 11.4m pupil, it will be the largest etendue telescope. The large focal plane can easily host up to 16.000 fibres. In addition, a gravity invariant focus for the central 10 arc-minutes is available to host a giant integral field unit (IFU). The 3 lenses corrector includes an ADC, and has good performance in the 360-1300 nm wavelength range. The top level science requirements were developed by a dedicated ESO working group, and one of the primary cases is high resolution spectroscopy of GAIA stars and, in general, how our Galaxy formed and evolves. The facility will therefore be equipped with both, high and low resolution spectrographs. We stress the importance of developing the telescope and instrument designs simultaneously. The most relevant R&D aspect is also briefly discussed.

scholarly journals What can the occult do for you?

2016 ◽  
Vol 11 (S321) ◽  
pp. 248-250
Author(s):  
B. W. Holwerda ◽  
W. C. Keel
Keyword(s):  
Interstellar Dust ◽  
Probability Function ◽  
Great Accuracy ◽  
Extinction Curve ◽  
Clear Understanding ◽  
Fine Scale ◽  
Grain Composition ◽  
Field Unit ◽  
Integral Field

AbstractInterstellar dust is still a dominant uncertainty in Astronomy, limiting precision in e.g., cosmological distance estimates and models of how light is re-processed within a galaxy. When a foreground galaxy serendipitously overlaps a more distant one, the latter backlights the dusty structures in the nearer foreground galaxy.Such an overlapping or occulting galaxy pair can be used to measure the distribution of dust in the closest galaxy with great accuracy. The STARSMOG program uses Hubble to map the distribution of dust in foreground galaxies in fine (<100 pc) detail. Integral Field Unit (IFU) observations will map the effective extinction curve, disentangling the role of fine-scale geometry and grain composition on the path of light through a galaxy.The overlapping galaxy technique promises to deliver a clear understanding of the dust in galaxies: geometry, a probability function of dimming as a function of galaxy mass and radius, and its dependence on wavelength.

Development of an integral field unit for a near-infrared multi-object imaging spectrograph SWIMS

2012 ◽  
Author(s):  
Shinobu Ozaki ◽  
Yutaro Kitagawa ◽  
Kentaro Motohara ◽  
Masahiro Konishi ◽  
Hidenori Takahashi ◽  
...  
Keyword(s):  
Near Infrared ◽  
Field Unit ◽  
Imaging Spectrograph ◽  
Integral Field ◽  
Object Imaging

scholarly journals What can the Occult do for you? STarlight Attenuation & Reddening Survey of Multiple Occulting Galaxies (STARSMOG)

2015 ◽  
Vol 11 (A29B) ◽  
pp. 173-175
Author(s):  
B. W. Holwerda ◽  
W. C. Keel
Keyword(s):  
Interstellar Dust ◽  
High Redshift ◽  
Cosmic Time ◽  
Great Accuracy ◽  
Clear Understanding ◽  
Grain Composition ◽  
Galaxy Type ◽  
Field Unit ◽  
Integral Field

AbstractInterstellar dust is still the dominant uncertainty in Astronomy, limiting precision in e.g., cosmological distance estimates and models of how light is re-processed within a galaxy. When a foreground galaxy serendipitously overlaps a more distant one, the latter backlights the dusty structures in the nearer foreground galaxy. Such an overlapping or occulting galaxy pair can be used to measure the distribution of dust in the closest galaxy with great accuracy. The STARSMOG program uses HST observation of occulting galaxy pairs to accurately map the distribution of dust in foreground galaxies in fine (<100 pc) detail. Furthermore, Integral Field Unit observations of such pairs will map the effective extinction curve in these occulting galaxies, disentangling the role of fine-scale geometry and grain composition on the path of light through a galaxy.The overlapping galaxy technique promises to deliver a clear understanding of the dust in galaxies: the dust geometry, a probability function of the amount of dimming as a function of galaxy type, its dependence on wavelength, and evolution of all these properties with cosmic time using distant, high-redshift pairs.

scholarly journals A panchromatic spatially resolved study of the inner 500 pc of NGC 1052 – II. Gas excitation and kinematics

2019 ◽  
Vol 489 (4) ◽  
pp. 5653-5668 ◽  
Author(s):  
L G Dahmer-Hahn ◽  
R Riffel ◽  
T V Ricci ◽  
J E Steiner ◽  
T Storchi-Bergmann ◽  
...  
Keyword(s):  
Large Scale ◽  
Near Infrared ◽  
Elliptical Galaxy ◽  
Field Of View ◽  
Spatially Resolved ◽  
Broad Component ◽  
Single Mechanism ◽  
Line Region ◽  
Nir Emission ◽  
Integral Field

ABSTRACT We map the optical and near-infrared (NIR) emission-line flux distributions and kinematics of the inner 320 × 535 pc2 of the elliptical galaxy NGC 1052. The integral field spectra were obtained with the Gemini Telescope using the GMOS-IFU and NIFS instruments, with angular resolutions of 0.88 and 0.1 arcsec in the optical and NIR, respectively. We detect five kinematic components: (1) and (2) two spatially unresolved components: a broad-line region visible in H α, with a full width at half-maximum (FWHM) of ∼3200 km s−1, and an intermediate broad component seen in the [O iii] λλ4959,5007 doublet; (3) an extended intermediate-width component with 280 km s−1 < FWHM < 450 km s−1 and centroid velocities up to 400 km s−1, which dominates the flux in our data, attributed either to a bipolar outflow related to the jets, rotation in an eccentric disc or to a combination of a disc and large-scale gas bubbles; (4) and (5) two narrow (FWHM < 150 km s−1) components, one visible in [O iii], and another visible in the other emission lines, extending beyond the field of view of our data, which is attributed to large-scale shocks. Our results suggest that the ionization within the observed field of view cannot be explained by a single mechanism, with photoionization being the dominant mechanism in the nucleus with a combination of shocks and photoionization responsible for the extended ionization.

scholarly journals GMOS IFU Observations of the Gas Kinematics in the Radio Galaxy Arp 102B

2009 ◽  
Vol 5 (S267) ◽  
pp. 395-395
Author(s):  
Guilherme d. S. Couto ◽  
Thaisa Storchi-Bergmann ◽  
Rogemar A. Riffel ◽  
D. J. Axon ◽  
A. Robinson
Keyword(s):  
Wavelength Range ◽  
Radio Galaxy ◽  
Field Of View ◽  
Trace Gas ◽  
Spiral Arms ◽  
Gas Kinematics ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Integral Field

The goal of this work is to map the gas excitation and kinematics in the inner ~ 2 kiloparsecs of the radio-galaxy Arp 102B. Though being classified as an E0 galaxy, Arp 102B shows a nuclear gas spiral (Fathi et al., in preparation). Previous studies of the gas kinematics in nuclear spirals have led to the conclusion that these structures usually trace gas inflows (Fathi et al. 2006; [Storchi-Bergmann et al. 2007; [Riffel et al. 2008). We have used integral field spectroscopy obtained with GMOS instrument of the Gemini North telescope to investigate the nature of the nuclear spiral arms. The spectra cover the wavelength range 4400–7300 Å over a field of view of 5.″5 × 3.″9 (2.7 kpc × 1.9 kpc).

scholarly journals KOOLS–IFU: Kyoto Okayama Optical Low-dispersion Spectrograph with optical-fiber Integral Field Unit

2019 ◽  
Vol 71 (5) ◽  
Author(s):  
Kazuya Matsubayashi ◽  
Kouji Ohta ◽  
Fumihide Iwamuro ◽  
Ikuru Iwata ◽  
Eiji Kambe ◽  
...  
Keyword(s):  
Optical Fiber ◽  
Gamma Ray ◽  
Field Of View ◽  
Resolving Power ◽  
Optimal Conditions ◽  
Total Field ◽  
Fiber Array ◽  
Field Unit ◽  
Low Dispersion ◽  
Integral Field

Abstract Observations of transient objects, such as short gamma-ray bursts and electromagnetic counterparts of gravitational wave sources, require prompt spectroscopy. To carry out prompt spectroscopy, we have developed an optical-fiber integral field unit (IFU) and connected it with an existing optical spectrograph, KOOLS. KOOLS–IFU was mounted on the Okayama Astrophysical Observatory 188 cm telescope. The fiber core and cladding diameters of the fiber bundle are 100 μm and 125 μm, respectively, and 127 fibers are hexagonally close-packed in the sleeve of the two-dimensional fiber array. We conducted test observations to measure the KOOLS–IFU performance and obtained the following conclusions: (1) the spatial sampling is ${2{^{\prime\prime}_{.}}34}$$\, \pm \,$${0{^{\prime\prime}_{.}}05}$ per fiber, and the total field of view is ${30{^{\prime\prime}_{.}}4}$$\, \pm \,$${0{^{\prime\prime}_{.}}65}$ with 127 fibers; (2) the observable wavelength and the spectral resolving power of the grisms of KOOLS are 4030–7310 Å and 400–600, 5020–8830 Å and 600–900, 4160–6000 Å and 1000–1200, and 6150–7930 Å and 1800–2400, respectively; and (3) the estimated limiting magnitude is 18.2–18.7 AB mag during 30 min exposure under optimal conditions.

The Integral Field Unit of the Near Infrared Spectrograph for JWST

2009 ◽  
pp. 21-26 ◽  
Author(s):  
S. Arribas ◽  
P. Ferruit ◽  
P. Jakobsen ◽  
T. Boeker ◽  
A. Bunker ◽  
...  
Keyword(s):  
Near Infrared ◽  
Field Unit ◽  
Integral Field
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