bHROS high spectral resolution observations of PN forbidden and recombination line profiles

A recent sounding rocket experiment has provided high spectral resolution line profiles across the solar disk. The objective of this experiment is to provide information on the systematic velocity fields at the base of the corona by observing the displacement, width and shape of EUV emission lines.

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High spectral resolution line profiles and images of comet Halley

Advances in Space Research ◽

10.1016/0273-1177(85)90097-3 ◽

1985 ◽

Vol 5 (12) ◽

pp. 279-282 ◽

Cited By ~ 10

Author(s):

F.L. Roesler ◽

F. Scherb ◽

K. Magee ◽

J. Harlander ◽

R.J. Reynolds ◽

...

Keyword(s):

Spectral Resolution ◽

High Spectral Resolution ◽

Line Profiles ◽

Comet Halley

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H2 2.12 μm Spectroscopy and Imaging of HH Objects

International Astronomical Union Colloquium ◽

10.1017/s0252921100023927 ◽

1989 ◽

Vol 120 ◽

pp. 302-302

Author(s):

H. Zinnecker ◽

R. Mundt ◽

A. Moneti ◽

T.R. Geballe ◽

W.J. Zealey

Keyword(s):

Spectral Resolution ◽

High Spatial Resolution ◽

Preliminary Test ◽

High Spectral Resolution ◽

Line Of Sight ◽

Line Profiles ◽

Ir Camera ◽

Fabry Perot ◽

Hh Objects ◽

Hh Object

We have obtained high spectral resolution observations of a number of Herbig-Haro (HH) objects in the H2 v=1-0 S(1) line at 2.12μm. Objects observed included HH1/2, HH7-11, HH19, HH32A, HH40, and HH43, all associated with jet-like features or collimated optical outflows. Here we present velocity-resolved 2.12μm spectroscopy for HH40 (an HH-objects moving close to the line of sight) an for HH43B (an HH-object moving close to the plane of the sky). The full set of observations including interpretation is given in Zinnecker et al. (1989). We also present high spatial resolution H2 2.12μm images of HH40 and HH43. The 2.12μm H2 line profiles were obtained with the UKIRT infrared Fabry-Perot system (effective resolution 30-35 km/s) using a diaphragm of diameter 11” for both HH40 and HH43. The H2 images were obtained with the IR-array imager at the CTIO 1.5m telescope through a narrowband filter centred on the v=1-0 S(1) line. The IR-camera used had 58x62 pixels and a resolution of 0.9”/pixel. The exposure time was 2x120sec and 5x60sec for HH40 and HH43, respectively. The images are sky subtracted, but not fiat fielded, and should be viewed as preliminary test images.

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Herschel/HIFI observations of molecular lines from young planetary nebulae

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312011222 ◽

2011 ◽

Vol 7 (S283) ◽

pp. 320-321

Author(s):

Valentín Bujarrabal ◽

Miguel Santander-García ◽

Javier Alcolea ◽

Rebeca Soria ◽

Keyword(s):

Spectral Resolution ◽

High Velocity ◽

Planetary Nebulae ◽

High Spectral Resolution ◽

Radiative Cooling ◽

Line Profiles ◽

Bipolar Outflows ◽

Molecular Lines ◽

Dense Flows

AbstractWe present results from systematic Herschel/HIFI observations of molecular lines in the FIR/sub-mm from young planetary nebulae. The high spectral resolution provided by the hetorodyne spectrometer HIFI allows properly studying the line profiles, whose structure corresponds to the various kinematics of the most massive nebular components, including fast bipolar outflows and slow shells. In particular, we have studied the excitation properties of the high-velocity (dense) flows. In some cases we find typical temperatures of the fast gas over 100-200 K, though in others it remains cool, ≲30K. We argue that the thermodynamics of the molecule-rich bipolar outflows is driven by fast radiative cooling, after the passage of the shock that accelerated it.

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Probing the atmosphere of HD189733b with the Na i and K i lines

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2435 ◽

2020 ◽

Vol 498 (1) ◽

pp. 1023-1033

Author(s):

E Keles ◽

D Kitzmann ◽

M Mallonn ◽

X Alexoudi ◽

L Fossati ◽

...

Keyword(s):

High Resolution ◽

High Altitude ◽

Spectral Resolution ◽

Absorption Lines ◽

High Spectral Resolution ◽

Transmission Spectra ◽

Line Profiles ◽

Line Broadening ◽

Atmospheric Processes ◽

Hot Jupiters

ABSTRACT High spectral resolution transmission spectroscopy is a powerful tool to characterize exoplanet atmospheres. Especially for hot Jupiters, this technique is highly relevant, due to their high-altitude absorption, e.g. from resonant sodium (Na i) and potassium (K i) lines. We resolve the atmospheric K i absorption on HD189733b with the aim to compare the resolved K i line and previously obtained high-resolution Na i-D line observations with synthetic transmission spectra. The line profiles suggest atmospheric processes leading to a line broadening of the order of ∼10 km/s for the Na i-D lines and only a few km/s for the K i line. The investigation hints that either the atmosphere of HD189733b lacks a significant amount of K i or the alkali lines probe different atmospheric regions with different temperature, which could explain the differences we see in the resolved absorption lines.

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Sun-as-a-star observations of the 2017 August 21 solar eclipse

Proceedings of the International Astronomical Union ◽

10.1017/s1743921319010019 ◽

2019 ◽

Vol 15 (S354) ◽

pp. 473-480

Author(s):

Ekaterina Dineva ◽

Carsten Denker ◽

Meetu Verma ◽

Klaus G. Strassmeier ◽

Ilya Ilyin ◽

...

Keyword(s):

Solar Eclipse ◽

Spectral Resolution ◽

Solar Disk ◽

State Of The Art ◽

Active Regions ◽

Spectral Lines ◽

High Spectral Resolution ◽

Line Profiles ◽

Stellar Spectra ◽

Limb Darkening

AbstractThe Potsdam Echelle Polarimetric and Spectroscopic Instrument (PEPSI) is a state-of-the-art, thermally stabilized, fiber-fed, high-resolution spectrograph for the Large Binocular Telescope (LBT) at Mt. Graham, Arizona. During daytime the instrument is fed with sunlight from the 10-millimeter aperture, fully automated, binocular Solar Disk-Integrated (SDI) telescope. The observed Sun-as-a-star spectra contain a multitude of photospheric and chromospheric spectral lines in the wavelength ranges 4200–4800 Å and 5300–6300 Å. One of the advantages of PEPSI is that solar spectra are recorded in the exactly same manner as nighttime targets. Thus, solar and stellar spectra can be directly compared. PEPSI/SDI recorded 116 Sun-as-a-star spectra during the 2017 August 21 solar eclipse. The observed maximum obscuration was 61.6%. The spectra were taken with a spectral resolution of ≈ 250000 and an exposure time of 0.3 s. The high-spectral resolution facilitates detecting subtle changes in the spectra while the Moon passes the solar disk. Sun-as-a-star spectra are affected by changing contributions due to limb darkening and solar differential rotation, and to a lesser extend by supergranular velocity pattern and the presence of active regions on the solar surface. The goal of this study is to investigate the temporal evolution of the chromospheric Na D doublet during the eclipse and to compare observations with synthetic line profiles computed with the state-of-the-art Bifrost code.

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