Suzaku Metal Abundance Patterns in the Outflow Region of M 82 and the Importance of Charge Exchange

Konami, Saori; Matsushita, Kyoko; Tsuru, Takeshi Go; Gandhi, Poshak; Tamagawa, Toru

doi:10.1093/pasj/63.sp3.s913

Cited by 27 publications

(44 citation statements)

References 47 publications

(62 reference statements)

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“…The presence of multiple hot gas components is common in many systems, especially starbursts (e.g., Konami et al 2011;Mineo et al 2012). However, the power of these components is very large in Mrk 34 and converting the soft band power to a star formation rate (SFR) using the L 0.5-2 :SFR scaling relation from Mineo et al (2012) implies a high SFR X-ray > 140 M yr −1 even when the scatter in the relation is accounted for.…”

Section: On the Origin Of The Soft X-ray Emissionmentioning

confidence: 99%

NuSTAR UNVEILS A COMPTON-THICK TYPE 2 QUASAR IN MrK 34

Gandhi

Lansbury

Alexander

et al. 2014

ApJ

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We present Nuclear Spectroscopic Telescope Array (NuSTAR) 3-40 keV observations of the optically selected Type 2 quasar (QSO2) SDSS J1034+6001 or Mrk 34. The high-quality hard X-ray spectrum and archival XMMNewton data can be fitted self-consistently with a reflection-dominated continuum and a strong Fe Kα fluorescence line with equivalent width >1 keV. Prior X-ray spectral fitting below 10 keV showed the source to be consistent with being obscured by Compton-thin column densities of gas along the line of sight, despite evidence for much higher columns from multiwavelength data. NuSTAR now enables a direct measurement of this column and shows that N H lies in the Compton-thick (CT) regime. The new data also show a high intrinsic 2-10 keV luminosity of L 2-10 ∼ 10 44 erg s −1 , in contrast to previous low-energy X-ray measurements where L 2-10 10 43 erg s −1 (i.e., X-ray selection below 10 keV does not pick up this source as an intrinsically luminous obscured quasar). Both the obscuring column and the intrinsic power are about an order of magnitude (or more) larger than inferred from pre-NuSTAR X-ray spectral fitting. Mrk 34 is thus a "gold standard" CT QSO2 and is the nearest non-merging system in this class, in contrast to the other local CT quasar NGC 6240, which is currently undergoing a major merger coupled with strong star formation. For typical X-ray bolometric correction factors, the accretion luminosity of Mrk 34 is high enough to potentially power the total infrared luminosity. X-ray spectral fitting also shows that thermal emission related to star formation is unlikely to drive the observed bright soft component below ∼3 keV, favoring photoionization instead.

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Section: On the Origin Of The Soft X-ray Emissionmentioning

confidence: 99%

NuSTAR UNVEILS A COMPTON-THICK TYPE 2 QUASAR IN MrK 34

Gandhi

Lansbury

Alexander

et al. 2014

ApJ

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“…We conclude that the LLS originates from gas expelled from the ISM of the nearby pair of dwarf galaxies, in particular tidally stripped gas during past or ongoing interactions between the two galaxies (e.g., Stierwalt et al 2015;Pearson et al 2016). While it is also possible that the gas comes from a starburst-driven wind out of one or both galaxies, we consider such a scenario less likely in light of the inferred high [Fe/α] relative abundances in these two components (e.g., Konami et al 2011;Mitsuishi et al 2013). 5.2.2 LLS at z abs = 0.43526 toward J0357−4812…”

Section: Lls At Z Abs = 036400 Toward J0248−4048mentioning

confidence: 99%

The Cosmic Ultraviolet Baryon Survey (CUBS) – III. Physical properties and elemental abundances of Lyman-limit systems at z < 1

Zahedy

Chen

Cooper

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a systematic investigation of physical conditions and elemental abundances in four optically thick Lyman-limit systems (LLSs) at z = 0.36 − 0.6 discovered within the Cosmic Ultraviolet Baryon Survey (CUBS). Because intervening LLSs at z < 1 suppress FUV light from background QSOs, an unbiased search of these absorbers requires a NUV-selected QSO sample, as achieved by CUBS. CUBS LLSs exhibit multi-component kinematic structure and a complex mix of multiphase gas, with associated metal transitions from multiple ionization states such as C II, C III, N iii, Mg II, Si II, Si III, O ii, O iii, O VI, and Fe ii absorption that span several hundred km s−1 in line-of-sight velocity. Specifically, higher column density components (log N(HI)/cm−2≳ 16) in all four absorbers comprise dynamically cool gas with 〈T〉 = (2 ± 1) × 104 K and modest non-thermal broadening of 〈bnt〉 = 5 ± 3 km s−1. The high quality of the QSO absorption spectra allows us to infer the physical conditions of the gas, using a detailed ionization modeling that takes into account the resolved component structures of H i and metal transitions. The range of inferred gas densities indicates that these absorbers consist of spatially compact clouds with a median line-of-sight thickness of $160^{+140}_{-50}$ pc. While obtaining robust metallicity constraints for the low-density, highly ionized phase remains challenging due to the uncertain $N\rm{(H\, {\small I})}$, we demonstrate that the cool-phase gas in LLSs has a median metallicity of $\mathrm{[\alpha /H]_{1/2}}=-0.7^{+0.1}_{-0.2}$, with a 16-84 percentile range of [α/H] = ( − 1.3, −0.1). Furthermore, the wide range of inferred elemental abundance ratios ([C/α], [N/α], and [Fe/α]) indicate a diversity of chemical enrichment histories. Combining the absorption data with deep galaxy survey data characterizing the galaxy environment of these absorbers, we discuss the physical connection between star-forming regions in galaxies and diffuse gas associated with optically thick absorption systems in the z < 1 circumgalactic medium.

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“…We note that super solar metallicities in hot winds driven by type II supernova explosions in starburst galaxies in conditions similar to those of our simulated galaxies are locally observed. For example, Konami et al (2011) observe the metallicity of hot X-ray gas of two to three times the solar value in M82. Martin et al (2002) find that the best-fit model for the hot X-ray gas metallicity in dwarf starburst galaxy NGC 1569 is solar, although a metallicity as high as five times solar still gives a χ 2 value only about 0.1% larger than the best-fit model; on the contrary, the model with 0.25 times solar has a much worse χ 2 value.…”

Section: Properties Of Embedding Interstellar Medium On Parsec Scalesmentioning

confidence: 99%

Diverse Properties of Interstellar Medium Embedding Gamma-Ray Bursts at the Epoch of Reionization

Cen

Kimm

2014

ApJ

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Analysis is performed on ultra-high-resolution large-scale cosmological radiation-hydrodynamic simulations to quantify, for the first time, the physical environment of long-duration gamma-ray bursts (GRBs) at the epoch of reionization. We find that, on parsec scales, 13% of GRBs remain in high-density ( 10 4 cm −3 ) low-temperature star-forming regions, whereas 87% of GRBs occur in low-density (∼10 −2.5 cm −3 ) high-temperature regions heated by supernovae. More importantly, the spectral properties of GRB afterglows, such as the neutral hydrogen column density, total hydrogen column density, dust column density, gas temperature, and metallicity of intervening absorbers, vary strongly from sight line to sight line. Although our model explains extant limited observationally inferred values with respect to circumburst density, metallicity, column density, and dust properties, a substantially larger sample of high-z GRB afterglows would be required to facilitate a statistically solid test of the model. Our findings indicate that any attempt to infer the physical properties (such as metallicity) of the interstellar medium (ISM) of the host galaxy based on a very small number (usually one) of sight lines would be precarious. Utilizing high-z GRBs to probe the ISM and intergalactic medium should be undertaken properly, taking into consideration the physical diversities of the ISM.

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Suzaku Metal Abundance Patterns in the Outflow Region of M 82 and the Importance of Charge Exchange

Cited by 27 publications

References 47 publications

NuSTAR UNVEILS A COMPTON-THICK TYPE 2 QUASAR IN MrK 34

NuSTAR UNVEILS A COMPTON-THICK TYPE 2 QUASAR IN MrK 34

The Cosmic Ultraviolet Baryon Survey (CUBS) – III. Physical properties and elemental abundances of Lyman-limit systems at z < 1

Diverse Properties of Interstellar Medium Embedding Gamma-Ray Bursts at the Epoch of Reionization

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Suzaku Metal Abundance Patterns in the Outflow Region of M 82 and the Importance of Charge Exchange

Cited by 27 publications

References 47 publications

NuSTAR UNVEILS A COMPTON-THICK TYPE 2 QUASAR IN MrK 34

NuSTAR UNVEILS A COMPTON-THICK TYPE 2 QUASAR IN MrK 34

The Cosmic Ultraviolet Baryon Survey (CUBS) – III. Physical properties and elemental abundances of Lyman-limit systems at z &lt; 1

Diverse Properties of Interstellar Medium Embedding Gamma-Ray Bursts at the Epoch of Reionization

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The Cosmic Ultraviolet Baryon Survey (CUBS) – III. Physical properties and elemental abundances of Lyman-limit systems at z < 1