2011A&A...525A.108H


Query : 2011A&A...525A.108H

2011A&A...525A.108H - Astronomy and Astrophysics, volume 525A, 108-108 (2011/1-1)

Searching for galactic hidden gas through interstellar scintillation: results from a test with the NTT-SOFI detector.

HABIBI F., MONIEZ M., ANSARI R. and RAHVAR S.

Abstract (from CDS):

Stars twinkle because their light propagates through the atmosphere. The same phenomenon is expected at a longer time scale when the light of remote stars crosses an interstellar molecular cloud, but it has never been observed at optical wavelength. In a favorable case, the light of a background star can be subject to stochastic fluctuations on the order of a few percent at a characteristic time scale of a few minutes. Our ultimate aim is to discover or exclude these scintillation effects to estimate the contribution of molecular hydrogen to the Galactic baryonic hidden mass. This feasibility study is a pathfinder toward an observational strategy to search for scintillation, probing the sensitivity of future surveys and estimating the background level. We searched for scintillation induced by molecular gas in visible dark nebulae as well as by hypothetical halo clumpuscules of cool molecular hydrogen (H2-He) during two nights. We took long series of 10s infrared exposures with the ESO-NTT telescope toward stellar populations located behind visible nebulae and toward the Small Magellanic Cloud (SMC). We therefore searched for stars exhibiting stochastic flux variations similar to what is expected from the scintillation effect. According to our simulations of the scintillation process, this search should allow one to detect (stochastic) transverse gradients of column density in cool Galactic molecular clouds of order of ∼3x10–5g/cm2/10000km. We found one light-curve that is compatible with a strong scintillation effect through a turbulent structure characterized by a diffusion radius Rdiff<100km in the B68 nebula. Complementary observations are needed to clarify the status of this candidate, and no firm conclusion can be established from this single observation. We can also infer limits on the existence of turbulent dense cores (of number density n>109cm–3) within the dark nebulae. Because no candidate is found toward the SMC, we are also able to establish upper limits on the contribution of gas clumpuscules to the Galactic halo mass. The limits set by this test do not seriously constrain the known models, but we show that the short time-scale monitoring for a few 106star x hour in the visible band with a >4m telescope and a fast readout camera should allow one to quantify the contribution of turbulent molecular gas to the Galactic halo. The LSST (Large Synoptic Survey Telescope) is perfectly suited for this search.

Abstract Copyright:

Journal keyword(s): dark matter - Galaxy: disk - Galaxy: halo - Galaxy: structure - local interstellar matter - ISM: molecules

Nomenclature: Fig. 10, Paragr. 5.4: [HMA2011] 4338 N=1.

Simbad objects: 9

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Number of rows : 9
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 OGLE SMC-SC6 148139 EB* 00 52 34.96 -72 50 01.2   17.34 17.42 17.44 17.39 ~ 8 0
2 SV* HV 1562 cC* 00 52 37.1330880600 -72 49 37.261412436   16.430 15.978   15.272 ~ 10 0
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10689 1
4 OGLE SMC-CEP-1968 cC* 00 52 54.0779273256 -72 47 42.700916112   17.864 17.331   16.596 ~ 7 0
5 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16759 1
6 NAME Circinus Region reg 14 49 -65.3           ~ 30 0
7 LDN 57 DNe 17 22 38.2 -23 49 34           ~ 306 1
8 [HMA2011] 4338 * 17 22 42.3 -23 48 57           ~ 1 0
9 LDN 327 DNe 18 16.9 -18 04           ~ 18 0

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2023.06.08-13:15:44

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