The Diffuse Interstellar Bands

Herbig, G. H.

doi:10.1146/annurev.astro.33.1.19

Cited by 242 publications

(394 citation statements)

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“…It is now generally believed that the DIBs are caused by free molecules in the gas phase (Herbig 1995), but despite many decades of effort by astronomers and molecular spectroscopists, there has been no match between any subset of the diffuse bands and the gas-phase laboratory spectrum of an individual molecule.…”

Section: Introductionmentioning

confidence: 99%

Rejection of the C[FORMULA][F][SUP]-[/SUP][INF]7[/INF][/F][/FORMULA] Diffuse Interstellar Band Hypothesis

McCall

Thorburn

Hobbs

et al. 2001

The Astrophysical Journal

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Using the new high-resolution (∼8 km s Ϫ1 ) echelle spectrograph on the 3.5 m telescope at the Apache Point Observatory, we have begun a high-sensitivity survey of the diffuse interstellar bands (DIBs) in a large sample of reddened stars. Now that we are 2 years into this long-term survey, our sample includes over 20 reddened stars that show at least one of the DIBs that had been suggested to be caused by C , based on the gas-phase Ϫ 7 measurement of the C spectrum by J. P. Maier's group. The high-quality astronomical data from this larger Ϫ 7 sample of stars, along with the spectroscopic constants from the new laboratory work recently reported by Maier's group, have enabled us to examine more carefully the agreement between C and the DIBs. We find that none is actually a stellar line. The two strongest DIBs attributed to C (l6270 and l4964) are not correlated in strength, Ϫ 7 so they cannot share the same carrier. On the whole, we find no evidence supporting the hypothesis that C is Ϫ 7 a carrier of the DIBs.

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Section: Introductionmentioning

confidence: 99%

Rejection of the C[FORMULA][F][SUP]-[/SUP][INF]7[/INF][/F][/FORMULA] Diffuse Interstellar Band Hypothesis

McCall

Thorburn

Hobbs

et al. 2001

The Astrophysical Journal

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“…In our Galaxy, such DIBs are quite commonly observed in high-resolution spectra of massive stars (Herbig 1995). There exist also measurements for the Small and Large Magellanic Clouds (Vladilo et al 1987;Ehrenfreund, P. et al, 2002;Cox et al 2006;Cox, N. L. J. et al, 2007;Welty et al 2006).…”

Section: Introductionmentioning

confidence: 74%

Time series of high-resolution spectra of SN 2014J observed with the TIGRE telescope

Jack¹,

Mittag²,

Schröder³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a time series of high resolution spectra of the Type Ia supernova 2014J, which exploded in the nearby galaxy M82. The spectra were obtained with the HEROŚ echelle spectrograph installed at the 1.2 m TIGRE telescope. We present a series of 33 spectra with a resolution of R ≈ 20, 000, which covers the important bright phases in the evolution of SN 2014J during the period from January 24 to April 1 of 2014. The spectral evolution of SN 2014J is derived empirically. The expansion velocities of the Si II P-Cygni features were measured and show the expected decreasing behaviour, beginning with a high velocity of 14,000 km/s on January 24. The Ca II infrared triplet feature shows a high velocity component with expansion velocities of > 20, 000 km/s during the early evolution apart from the normal component showing similar velocities as Si II. Further broad P-Cygni profiles are exhibited by the principal lines of Ca II, Mg II and Fe II. The TIGRE SN 2014J spectra also resolve several very sharp Na I D doublet absorption components. Our analysis suggests interesting substructures in the interstellar medium of the host galaxy M82, as well as in our Milky Way, confirming other work on this SN. We were able to identify the interstellar absorption of M82 in the lines of Ca II H & K at 3933 and 3968Å as well as K I at 7664 and 7698Å. Furthermore, we confirm several Diffuse Interstellar Bands, at wavelengths of 6196, 6283, 6376, 6379 and 6613Å and give their measured equivalent widths.

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“…These bands are absorption lines observed in the optical and infrared spectra of reddened stars (Herbig 1995); the strength of some of them roughly correlated with the color excess produced by interstellar reddening. We measured the equivalent widths (EW s) of DIBs located at 5780, 5797 and 8620 Å (EW = 0.30 ± 0.01, 0.08 ± 0.01 and 0.20 ± 0.01 Å, respectively) and used the relations given by Munari (2000) and Weselak et al (2008) to estimate E(B − V) = 0.55 ± 0.15.…”

Section: Spectral Energy Distribution Reddening and Distancementioning

confidence: 90%

Fundamental parameters of the close interacting binary HD 170582 and its luminous accretion disc

Mennickent

Djurašević

Cabezas

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present a spectroscopic and photometric study of the Double Period Variable HD 170582. Based on the study of the ASAS V-band light curve we determine an improved orbital period of 16.87177 ± 0.02084 days and a long period of 587 days. We disentangled the light curve into an orbital part, determining ephemerides and revealing orbital ellipsoidal variability with unequal maxima, and a long cycle, showing quasi-sinusoidal changes with amplitude ∆V= 0.1 mag. Assuming synchronous rotation for the cool stellar component and semi-detached configuration we find a cool evolved star of M 2 = 1.9 ± 0.1 M , T 2 = 8000 ± 100 K and R 2 = 15.6 ± 0.2 R , and an early B-type dwarf of M 1 = 9.0 ± 0.2 M . The B-type star is surrounded by a geometrically and optically thick accretion disc of radial extension 20.8 ± 0.3 R contributing about 35% to the system luminosity at the V band. Two extended regions located at opposite sides of the disc rim, and hotter than the disc by 67% and 46%, fit the light curve asymmetries. The system is seen under inclination 67.4 ± 0.4 degree and it is found at a distance of 238 ± 10 pc. Specially interesting is the double line nature of He i 5875; two absorption components move in anti-phase during the orbital cycle; they can be associated with the shock regions revealed by the photometry. The radial velocity of one of the He i 5875 components closely follows the donor radial velocity, suggesting that the line is formed in a wind emerging near the stream-disc interacting region.

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The Diffuse Interstellar Bands

Cited by 242 publications

References 0 publications

Rejection of the C[FORMULA][F][SUP]-[/SUP][INF]7[/INF][/F][/FORMULA] Diffuse Interstellar Band Hypothesis

Rejection of the C[FORMULA][F][SUP]-[/SUP][INF]7[/INF][/F][/FORMULA] Diffuse Interstellar Band Hypothesis

Time series of high-resolution spectra of SN 2014J observed with the TIGRE telescope

Fundamental parameters of the close interacting binary HD 170582 and its luminous accretion disc

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