Neutral Hydrogen Clouds in the M81/M82 Group

Chynoweth, Katie M.; Langston, G. I.; Yun, Min S.; Lockman, Felix J.; Rubin, Kate H. R.; Scoles, Sarah

doi:10.1088/0004-6256/135/6/1983

Cited by 87 publications

(130 citation statements)

References 24 publications

(45 reference statements)

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“…Stripped gas due to tidal interactions between neighboring galaxies is a likely explanation for the dynamically complex Mg II absorbers found in group or cluster environments (e.g. Chynoweth et al, 2008;Marasco et al, 2016), which also results in H I depleted galaxies in these Fig. 5 Comparison of galaxy and Mg II absorption gas kinematics observed in a group of galaxies at z = 0.5624 (Gauthier, 2013).…”

Section: Kinematicsmentioning

confidence: 99%

The Circumgalactic Medium in Massive Halos

Chen

2017

Gas Accretion Onto Galaxies

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This chapter presents a review of the current state of knowledge on the cool (T ∼ 10 4 K) halo gas content around massive galaxies at z ≈ 0.2 − 2. Over the last decade, significant progress has been made in characterizing the cool circumgalactic gas in massive halos of M h ≈ 10 12−14 M at intermediate redshifts using absorption spectroscopy. Systematic studies of halo gas around massive galaxies beyond the nearby universe are made possible by large spectroscopic samples of galaxies and quasars in public archives. In addition to accurate and precise constraints for the incidence of cool gas in massive halos, detailed characterizations of gas kinematics and chemical compositions around massive quiescent galaxies at z ≈ 0.5 have also been obtained. Combining all available measurements shows that infalling clouds from external sources are likely the primary source of cool gas detected at d > ∼ 100 kpc from massive quiescent galaxies. The origin of the gas closer in is currently less certain, but SNe Ia driven winds appear to contribute significantly to cool gas found at d < 100 kpc. In contrast, cool gas observed at d < ∼ 200 kpc from luminous quasars appears to be intimately connected to quasar activities on parsec scales. The observed strong correlation between cool gas covering fraction in quasar host halos and quasar bolometric luminosity remains a puzzle. Combining absorption-line studies with spatially-resolved emission measurements of both gas and galaxies is the necessary next step to address remaining questions.

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Section: Kinematicsmentioning

confidence: 99%

The Circumgalactic Medium in Massive Halos

Chen

2017

Gas Accretion Onto Galaxies

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“…One such example is the extended tidal structures seen in the nearby galaxygroupM81 (Yun et al 1994;Chynoweth et al 2008). Strong dynamical disruption in the spectral profiles of the cold gas in HCG44 and HCG 92 indicates that their origin is related to the transformation of the ISM of individual galaxies into the IGrM.…”

Section: Nature and Origin Of The Diffuse Extended Gas In Hcgsmentioning

confidence: 99%

Distribution of Faint Atomic Gas in Hickson Compact Groups

Borthakur

Yun

Verdes–Montenegro

et al. 2015

ApJ

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We present 21 cm H I observations of four Hickson Compact Groups (HCGs) with evidence for a substantial intragroup medium using the Robert C. Byrd Green Bank Telescope (GBT).5 By mapping H I emission in a region of 25′ × 25′ (140-650 kpc) surrounding each HCG, these observations provide better estimates of H I masses. In particular, we detected 65% more H I than that detected in the Karl G. Jansky Very Large Array (VLA) imaging of HCG 92. We also identify whether the diffuse gas has the same spatial distribution as the highsurface brightness (HSB) H I features detected in the VLA maps of these groups by comparing the H I strengths between the observed and modeled masses based on VLA maps. We found that the H I observed with the GBT has a similar spatial distribution to the HSB structures in HCG31 and HCG 68. Conversely, the observed H I distributions in HCG44 and HCG 92 were extended and showed significant offsets from the modeled masses. Most of the faint gas in HCG 44 lies to the northeast-southwest region and in HCG 92 lies in the northwest region of their respective groups. The spatial and dynamical similarities between the total (faint+HSB) and the HSB H I indicate that the faint gas is of tidal origin. We found that the gas will survive ionization by the cosmic UV background and the escaping ionizing photons from the star-forming regions and stay primarily neutral for at least 500 Myr.

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“…As a result, L FIR /M gas is estimated to be 1.4 L M −1 with the total gas mass (M H 2 + M H I ) of 3 × 10 9 M (Brouillet et al 1991;Chynoweth et al 2008). Siebenmorgen et al (1999) have defined active (Seyfert and starburst) and inactive (normal) galaxies according to L FIR /M gas and the number of the dust component.…”

Section: Spectral Energy Distribution Of M 81mentioning

confidence: 99%

Kiloparsec-scale star formation law in M 81 and M 101 based on AKARI far-infrared observations

Suzuki¹,

Kaneda²,

Onaka³

et al. 2010

A&A

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Aims. We assess the relationships between the surface densities of the gas and star formation rate (SFR) within spiral arms of the nearby late-type spiral galaxies M 81 and M 101. By analyzing these relationships locally, we empirically derive a kiloparsec scale Kennicutt-Schmidt Law (Σ SFR ∝ Σ N gas ). Methods. Both M 81 and M 101 were observed with the Far-Infrared Surveyor (FIS) aboard AKARI in four far-infrared bands at 65, 90, 140, and 160 μm. Results. The spectral energy distributions of the whole galaxies show the presence of the cold dust component (T C ∼ 20 K) in addition to the warm dust component (T W ∼ 60 K). We deconvolved the cold and warm dust emission components spatially by making the best use of the multi-band photometric capability of the FIS. The cold and warm dust components show power-law correlations in various regions, which can be converted into the gas mass and the SFR, respectively. We find a power-law correlation between the gas and SFR surface densities with significant differences in the power-law index N between giant H ii regions (N = 1.0 ± 0.5) and spiral arms (N = 2.2 ± 0.2) in M 101. The power-law index for spiral arms in M 81 is similar (N = 1.9 ± 0.4) to that of spiral arms in M 101. Conclusions. The power-law index is not always constant within a galaxy. The difference can be attributed to the difference in the star formation processes on a kiloparsec scale. N 2 seen in the spiral arms in M 81 and M 101 supports the scenario of star formation triggered by cloud-cloud collisions enhanced by a spiral density wave, while N 1 derived in giant H ii regions in M 101 suggests the star formation induced by the Parker instability triggered by high-velocity H i gas infall. The present method can be applied to a large galaxy sample for which the AKARI All Sky Survey provides the same 4 far-infrared band data.

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Neutral Hydrogen Clouds in the M81/M82 Group

Cited by 87 publications

References 24 publications

The Circumgalactic Medium in Massive Halos

The Circumgalactic Medium in Massive Halos

Distribution of Faint Atomic Gas in Hickson Compact Groups

Kiloparsec-scale star formation law in M 81 and M 101 based on AKARI far-infrared observations

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