adsabs/AstroCLIMB huggingface dataset:
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: Model fitting for different species. Continued from Figure 8. Note: In each panel, the spectrum between two neighboring upper ticks is an independent frequency segment containing transitions of the corresponding species. The solid red line represents the model fitting of the corresponding species, while the dashed line includes the contributions of all modeled molecular species (Table 2) and RRLs (see Section 4 for details). The x-axis is in units of megahertz. Each spectrum has been smoothed to a spectral resolution of 183 kHz.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption:                         Model fitting for CH3OH (upper panel) and 13CH3OH (lower panel) as an example. Spectra at different transitions are spliced together with segments marked by the gray ticks on the top axis. The x-axis is in units of megahertz with a channel width of 91.553 kHz (no smoothing applied). The solid red line represents the model fitting of the corresponding species, while the dashed line includes the contributions of all of the modeled molecular species (Table 2) and RRLs (see Section 4 for details). See Figure 9 for other species.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: An example of comparison between the spectra of this survey in blue and of Rizzo et al. (2017) in orange. The spectrum shown here has been smoothed to have the same spectral resolution of Rizzo et al. (2017). The red line represents the results of model fitting (Section 4). The bottom purple strips denote the detected RRLs. The yellow strips denote the molecular lines, which have also been firmly detected and resolved by Rizzo et al. (2017). The green strips denote the molecular lines detected by TMRT 65 m but have not been detected by Rizzo et al. (2017). The red strips denote the lines of C2H5CN υ13/υ21. The x-axis is the frequency, which has been converted to the rest frame of Orion KL with a V LSR of 6 km s−1 (Section 2.3).
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: The spectra of the 42,732/42,735 doublet observed in three different days. The fake signals appeared only once under an unknown particular situation, and no such phenomena happened during other observation setups (Section 3.4). The fake doublets are kept in the spectrum shown in Figure 4.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: Upper: groups of spectral components (Table 2) by K-means (Section 4.2.3). Lower: the number of spectral components with ΔV (in units of kilometers per second) in three different ranges.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: The rotational diagram of E-CH3OH υ  t  = 1.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: Pie diagrams to compare the number of molecular lines and RRLs of this survey with and without detection by R17 (Rizzo et al. 2017).
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1351A.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1317.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1365.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1316.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1316C.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1341.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1326.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1350.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1380.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Comparison between the Fornax galaxies and field galaxies with M star > 109 M ⊙: relationships between the offsets from the main sequence of star-forming galaxies with gas fractions, ﹩{R}_{{{\rm{H}}}_{2}}﹩, and SFEs. Symbols and lines are the same as in Figure 6. Our Fornax sample has lower gas fractions and higher ﹩{R}_{{{\rm{H}}}_{2}}﹩ and SFEs than the field galaxies at Δ(MS) ∼ −1.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: The relationship between the clustocentric distance with (a) R 5,sky and (b) R 5,PSD and between the accretion phase with (c) R 5,sky and (d) R 5,PSD. The median values for each bin of the clustocentric distance are indicated with black filled circles. The upper and lower caps indicate the third and first quartiles of R 5,sky or R 5,PSD in each clustocentric distance or accretion phase bin, respectively. The Spearman’s rank-order correlation coefficient r and the p-value are shown on the lower left corner of each panel in purple.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: The relationships between R 5,PSD with the key quantities [Δ(Field) values]. Symbols are the same as in Figure 10. R 5,PSD positively correlates to ﹩{\mu }_{{{\rm{H}}}_{2}}﹩ and negatively correlates to SFEgas.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1437B.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1436.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1425.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1386.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1406.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1387.
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: The similar observed efficiency (with E iso/E k from the X-ray afterglow) and theoretically predicted efficiency (from the prompt emission or the optical afterglow) of the photosphere emission model for the bursts after GRB 110213A. (a) The distribution of E ratio (﹩{E}_{\mathrm{ratio}}={[{({E}_{{\rm{p}}}/2.7k)}^{4}\ast {(4\pi {r}_{1}^{2}{ac})}^{}/{E}_{\mathrm{iso}}]}^{1/3}﹩, from the prompt emission) and E iso/E k for the ϵ  γ  ≲ 50% sample (see Table 2). They are found to be centered around the equal-value line, and have a linear correlation (reduced χ 2 = 0.172). The dispersion is likely to be caused by the estimation errors for E k, since many X-ray afterglow light curves are not power laws with slopes of −1. (b) and (c) The X-ray afterglow light curves for the bursts (seven bursts) with almost the same E ratio and E iso/E k (see Table 5). We find that all of these light curves do have a power-law shape with a slope of ∼−1. (d) The distributions of E ratio, E iso/E k, and ﹩{({R}_{\mathrm{ph}}/{R}_{s})}^{-2/3}﹩ for the sample (six bursts; see Table 2), with detections of the peak time of the optical afterglow (to estimate Γ and thus ﹩{({R}_{\mathrm{ph}}/{R}_{s})}^{-2/3}﹩). It is found that one burst has almost the same values for these three quantities, and that the five other bursts have almost the same values for two quantities (reduced χ 2 = 0.089 for all 12 markers). (e) The consistent efficiency from the observations (with E iso/E  k ) and the prediction from the photosphere emission model (with η/Γ) for the ϵ  γ  ≳ 50% sample, with detections of the peak time of the optical afterglow (seven bursts; see Table 3; reduced χ 2 = 0.120).
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: The ﹩{E}_{{\rm{p}}}\propto {({E}_{\mathrm{iso}})}^{1/4}﹩ and ﹩{E}_{{\rm{p}}}\propto {({L}_{\mathrm{iso}})}^{1/4}﹩ relations for the GRBs with the highest prompt efficiency ϵ  γ  (ϵ  γ  ≳ 80%; see Table 1). (a) The E iso and calculated L X,11h (the late-time X-ray afterglow luminosity at 11 hr) distribution for the whole GRB sample used (117 bursts, after GRB 110213A) with redshift. The red stars with the smallest L X,11h represent the bursts with the highest prompt efficiency. (b) The E p and E iso distribution for the 15 long GRBs selected. The best-fit result is log (E p) ﹩=\,2.54+0.25\mathrm{log}﹩ (E iso ), which is quite consistent with the ﹩{E}_{{\rm{p}}}\propto {({E}_{\mathrm{iso}})}^{1/4}﹩ relation predicted by the photosphere (thermal) emission model. (c) Comparison of the E p and E iso distributions for the selected GRBs (red stars) and the large sample of long GRBs (yellow circles; see Figure 3 in Zhang et al. 2018b). Obviously, the dispersion of the selected GRBs is quite small (reduced χ 2 = 0.009) relative to that of the large sample (reduced χ 2 = 0.035). The black dotted line shows the Amati relation (Amati et al. 2002) for the large sample. (d) Comparison of the E p − L iso distribution (red stars) and the E p − E iso distribution (blue stars) for the selected GRBs. Likewise, the ﹩{E}_{{\rm{p}}}\propto {({L}_{\mathrm{iso}})}^{1/4}﹩ relation exists. The best-fit result is log (E p) ﹩=2.75+0.23\mathrm{log}﹩ (L iso). The dispersion (reduced χ 2 = 0.012) is found to be similar to that of ﹩{E}_{{\rm{p}}}\propto {({E}_{\mathrm{iso}})}^{1/4}﹩.
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: The tight correlation of ﹩{\rm{\Gamma }}\propto {E}_{\mathrm{iso}}^{1/8}{E}_{{\rm{p}}}^{1/2}/{\left({T}_{90}\right)}^{1/4}﹩ to estimate Γ, which we derived using the same efficiency of E ratio and ﹩{({R}_{\mathrm{ph}}/{R}_{s})}^{-2/3}﹩ as in the ϵ  γ  ≲ 50% case (see Table 6). (a) The distribution of E ratio and ﹩{({R}_{\mathrm{ph}}/{R}_{s})}^{-2/3}﹩ for the selected ϵ  γ  ≲ 50% sample (based on E ratio ≤ 0.9; 24 bursts; reduced χ 2 = 0.239). (b) The distributions of E ratio and ﹩{({R}_{\mathrm{ph}}/{R}_{s})}^{-2/3}﹩ for the two subsamples with smaller E p errors (dE p/E p ≤ 0.2; blue circles; reduced χ 2 = 0.025) and larger E p errors (dE p/E p ≥ 0.2; purple triangles; reduced χ 2 = 0.228), respectively. (c) A comparison of the Γ obtained from the optical afterglow (for 47 bursts, from Ghirlanda et al. 2018) and the Γ obtained from the prompt emission (orange triangles for ﹩{\rm{\Gamma }}={10}^{3.33}{L}_{\mathrm{iso}}^{0.46}{E}_{{\rm{p}}}^{-0.43}﹩ and blue circles for ﹩{\rm{\Gamma }}=17\cdot {E}_{\mathrm{iso}}^{1/8}{E}_{{\rm{p}}}^{1/2}/{\left({T}_{90}\right)}^{1/4}﹩). (d) The distribution of ﹩{[{E}_{{\rm{p}}}/{\left({T}_{90}\right)}^{1/2}]}^{4/3}﹩ and ﹩{T}_{p}^{}/(1+z)﹩ for 35 bursts (reduced χ 2 = 0.100). (e) The slightly different constants for the ϵ  γ  ≲ 50% case (Const = 19.67, reduced χ 2  = 0.034; Const = 16.75, purple triangles, reduced χ 2  = 0.048) and the ϵ  γ  ≳ 50% case (Const = 16.75).
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: The different distributions of E p and E iso for the two distinguished samples (ϵ  γ  ≳ 50% and ϵ  γ  ≲ 50%; see Tables 2 and 3) for the long GRBs. (a) The E p and E iso distribution for the bursts after GRB 110213A (117 bursts, with L X,11h derived in this work). For the ϵ  γ  ≳ 50% sample (red circles), the best-fit result is log (E p) ﹩=2.47+0.25\mathrm{log}﹩ (E iso) (reduced χ 2 = 0.039; for the dotted black line of the typical Amati relation, reduced χ 2 = 0.079), which is consistent with the predicted ﹩{E}_{{\rm{p}}}\propto {({E}_{\mathrm{iso}})}^{1/4}﹩ from the photosphere emission model. For the ϵ  γ  ≲ 50% sample (blue and cyan circles), the upmost distribution is found around ﹩\mathrm{log}﹩ (E p) ﹩=2.54+0.25\mathrm{log}﹩ (E iso), and the best-fit result is log (E p) ﹩=\,2.31+0.26\mathrm{log}﹩ (E iso) (reduced χ 2 = 0.076; for the typical Amati relation, reduced χ 2 = 0.113), much below that. (b) The E p and E iso distribution for the bursts before GRB 110213A (46 bursts, with L X,11h given in D’Avanzo et al. 2012). Different distributions of E p and E iso for the two distinguished samples (ϵ  γ  ≳ 50% and ϵ  γ  ≲ 50%) are also found, similar to the distributions for the bursts after GRB 110213A.
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: Comparison of Γ as obtained from ﹩{\rm{\Gamma }}\propto {E}_{\mathrm{iso}}^{1/8}{E}_{{\rm{p}}}^{1/2}/{\left({T}_{90}\right)}^{1/4}﹩ and from ﹩{\rm{\Gamma }}={10}^{3.33}{L}_{\mathrm{iso}}^{0.46}{E}_{{\rm{p}}}^{-0.43}﹩ (see Tables 6 and 1). (a) Comparison of the Γ obtained from the optical afterglow and the Γ obtained from the prompt emission (orange triangles for ﹩{\rm{\Gamma }}={10}^{3.33}{L}_{\mathrm{iso}}^{0.46}{E}_{{\rm{p}}}^{-0.43}﹩ and blue circles for ﹩{\rm{\Gamma }}\propto {E}_{\mathrm{iso}}^{1/8}{E}_{{\rm{p}}}^{1/2}/{\left({T}_{90}\right)}^{1/4}﹩) for the better sample (35 bursts) in Figure 7(d). The different constants are used for the ϵ  γ  ≳ 50% and ϵ  γ  ≲ 50% subsamples. (b) Comparison of Γ as obtained from ﹩{\rm{\Gamma }}={10}^{3.33}{L}_{\mathrm{iso}}^{0.46}{E}_{{\rm{p}}}^{-0.43}﹩ and from ﹩{\rm{\Gamma }}\propto {E}_{\mathrm{iso}}^{1/8}{E}_{{\rm{p}}}^{1/2}/{\left({T}_{90}\right)}^{1/4}﹩ for the ϵ  γ  ≲ 50% (cyan triangles; reduced χ 2 = 0.043), the ϵ  γ  ≳ 50% (orange circles; reduced χ 2 = 0.046), and the high-efficiency (ϵ  γ  ≳ 80%; red stars; reduced χ 2 = 0.017) subsamples. Obviously, these two estimations are consistent with each other, since they can be transferred with ﹩{E}_{{\rm{p}}}\propto {({E}_{\mathrm{iso}})}^{1/4}﹩. (c) The ﹩{T}_{90}\propto {({L}_{\mathrm{iso}})}^{-0.5}﹩ correlation (reduced χ 2 = 0.174) found for the high-efficiency subsample (ϵ  γ  ≳ 80%).