Accurate measurement of interstellar hydrogen as the target of hadronic gamma rays Yasuo Fukui Nagoya University Southern Observatories CTA meeting April.

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Presentation transcript:

Accurate measurement of interstellar hydrogen as the target of hadronic gamma rays Yasuo Fukui Nagoya University Southern Observatories CTA meeting April 16-17, 2015, Adelaide 1

ISM Interstellar medium ISM between stars ISM consists of gas and dust Mgas/Mdust is 100, dust grains include most of the heavy elements; H:He:CNO = 1:10 -1 :10 -4 Gas consists of neutral and ionized components Neutral is dominant, related to star formation Neutral consists of molecular and atomic gas 1951 discovery of 21cm HI 1970 discovery of 2.6mm CO [H2 has no suitable transition] 2

HI is assumed to be optically thin in text books

Molecular vs. atomic HI gas: average density 1 cm-3, Tk=125K “assumption, 21cm line optically thin” --NHI=1.8e18 WHI Dark gas: gamma rays (pp reaction    ), dust extinction “cannot be seen in HI or CO” --CO-free H2? H2 gas: density 1000 cm-3, Tk=10K “CO 2.6mm line via Xco factor” --NH2=Xco Wco (factor of 2 uncertainty) 4

Kalberla Courtesy of Legacy Archive for Microwave Background Data Analysis The Leiden/Argentine/Bonn Galactic HI Survey HI LAB 5

GeV Gamma rays

Planck Collaboration, arXiv: CO surveys : CfA + NANTEN

Isabelle Grenier et al. Science 2005 Column density of dark gas ~ /cm 2 8

Nearby cloud without background source [Fukui+ 2014]

MBM 53, 54, 55 tau353-WHI 相関プロット HI dust correlation is bad Planck sub-mm data 10

MBM 53, 54, 55 tau353-WHI 相関プロット HI dust correlation is bad Planck sub-mm data 11 Td highest HI is thin With Td decrease HI becomes thick Fukui+ 2014; 2015

Fig. 3 Ts=10, 20, 30, …, 100 K

All sky Planck tau353: Fukui+2015 masked in gray [double HI profiles/H  /CO/Plane]

Excess NHI =“Dark gas”

Planck Collaboration, arXiv:

HI becomes dark at higher density Goldsmith et al

Step 1 We estimate the W(HI) range Step 2 Estimating a conversion factor form W(HI) to NH using linier fitting Step 3 We apply the correction Tau 353 vs. W(HI)

(left) Image: Total interstellar proton column density, contours: TeV γ-rays (Aharonian+07) (Right) Azimuthal plots Fukui, Sano+15 in prep. Vela Jr. total ISM protons & TeV γ-rays

Vela Jr. total ISM protons & TeV γ-rays (optically thick HI corrected) (left) Image: Total interstellar proton column density, contours: TeV γ-rays (Aharonian+07) (Right) Azimuthal plots Fukui, Sano+15 in prep.

RX J : Interstellar proton vs. TeV gamma rays Fukui et al HI + 2H 2 24

Dark HI SE Cloud (Self-Absorption) 25

26 HI self absorption

Very accurate measurement of both atomic/molecular hydrogen has become possible by “truly optically thin HI” HI gas: average density 1 cm-3, Tk=125K “assumption, 21cm line optically thin” --NHI=1.8e18 x WHI but HI is optically thick Dark gas: gamma rays (pp reaction    ), dust extinction. CTA will play a major role H2 gas: density 1000 cm-3, Tk=10K “CO 2.6mm line via Xco factor” --NH2=Xco x Wco (factor of 2 uncertainty) 27