adsabs/AstroCLIMB huggingface dataset:
Paper: Follow-up Observations of Apparently One-off Sources from the Parkes Telescope
Authors: Songbo Zhang, Xuan Yang
Figure caption: Profiles and dynamic spectra for examples of detected pulses from three repeating sources. The bursts are plotted after being dedispersed using DMs of 127.2 pc cm−3 for (a) J0808−32, 186.4 pc cm−3 for (b) SPC 991113, and 225.8 pc cm−3 for (c) J1709−43. (a) is the Parkes UWL data, while (b) and (c) are the Multibeam data.
Paper: Optical Continuum Reverberation Mapping of a Candidate IMBH in a Nearby Seyfert 1 Galaxy
Authors: Wenwen Zuo, Hengxiao Guo, Jingbo Sun, Qi Yuan, Paulina Lira, Minfeng Gu, Philip G. Edwards, Alok C. Gupta, Shubham Kishore, Jamie Stevens, Tao An, Zhen-Yi Cai, Hai-Cheng Feng, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, Sha-Sha Li, Mar Mezcua, Luka Č. Popović, Mouyuan Sun, Tushar Tripathi, Vivian U, Oliver Vince, Jianguo Wang, Junxian Wang, Shu Wang, Xuebing Wu, Zhenya Zheng
Figure caption: Upper panel: spectra of J0249−0815 from SDSS and Palomar P200 in the rest frame. The absolute flux of two original spectra is shifted upward by 1 × 10−16 erg s−1 cm−2 Å−1 for better demonstration. Middle panel: host-AGN decomposition with a PCA method. Lower panel: spectral fitting for the continuum-subtracted Hα emission-line region. The blue line is the overall model consisting of Gaussian profiles: red lines are broad components for the Hα line, and green lines represent narrow emission lines, respectively. All these fits are based on PyQSOFit.
Paper: Optical Continuum Reverberation Mapping of a Candidate IMBH in a Nearby Seyfert 1 Galaxy
Authors: Wenwen Zuo, Hengxiao Guo, Jingbo Sun, Qi Yuan, Paulina Lira, Minfeng Gu, Philip G. Edwards, Alok C. Gupta, Shubham Kishore, Jamie Stevens, Tao An, Zhen-Yi Cai, Hai-Cheng Feng, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, Sha-Sha Li, Mar Mezcua, Luka Č. Popović, Mouyuan Sun, Tushar Tripathi, Vivian U, Oliver Vince, Jianguo Wang, Junxian Wang, Shu Wang, Xuebing Wu, Zhenya Zheng
Figure caption: Scaling of the g − z continuum lag as a function of AGN luminosity at 5100 Å (left panel) and BH mass (right panel), for 10 nearby AGNs having multiband continuum RM spanning the g to z bands. The best linear fits are shown in green lines with 1σ uncertainty (light gray region). The vertical red dashed lines correspond to the AGN continuum luminosity at 5100 Å obtained from spectral decomposition and single-epoch BH mass estimates based on the Hα component, respectively. The horizontal red dotted lines in both panels indicate the predicted continuum lags (∼1.6 to 3.3 hr) between the g and z bands in J0249−0815.
Paper: Optical Continuum Reverberation Mapping of a Candidate IMBH in a Nearby Seyfert 1 Galaxy
Authors: Wenwen Zuo, Hengxiao Guo, Jingbo Sun, Qi Yuan, Paulina Lira, Minfeng Gu, Philip G. Edwards, Alok C. Gupta, Shubham Kishore, Jamie Stevens, Tao An, Zhen-Yi Cai, Hai-Cheng Feng, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, Sha-Sha Li, Mar Mezcua, Luka Č. Popović, Mouyuan Sun, Tushar Tripathi, Vivian U, Oliver Vince, Jianguo Wang, Junxian Wang, Shu Wang, Xuebing Wu, Zhenya Zheng
Figure caption: Light curves of J0249−0815. Two-night photometry is performed using the MuSCAT four-channel imager. Night 1 and the first half of Night 2 are observed by MuSCAT 3 at the Haleakalā Observatory, Hawaii, while the rest is observed by MuSCAT 4 at Siding Spring Observatory, Australia. The single exposure times of ﹩{g}^{{\prime} }﹩, ﹩{r}^{{\prime} }﹩, ﹩{i}^{{\prime} }﹩, and z  s  are 100 s, 25 s, 100 s, and 100 s. Their photometric errors are 1.0%, 1.8%, 0.8%, and 1.3%, respectively. No significant variations were detected during this monitoring period.
Paper: Optical Continuum Reverberation Mapping of a Candidate IMBH in a Nearby Seyfert 1 Galaxy
Authors: Wenwen Zuo, Hengxiao Guo, Jingbo Sun, Qi Yuan, Paulina Lira, Minfeng Gu, Philip G. Edwards, Alok C. Gupta, Shubham Kishore, Jamie Stevens, Tao An, Zhen-Yi Cai, Hai-Cheng Feng, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, Sha-Sha Li, Mar Mezcua, Luka Č. Popović, Mouyuan Sun, Tushar Tripathi, Vivian U, Oliver Vince, Jianguo Wang, Junxian Wang, Shu Wang, Xuebing Wu, Zhenya Zheng
Figure caption: Host image decomposition based on the DECaLS g-band image using GALFIT. The plots from left to right are the original data, the best-fit model, the fitting residuals (data−model), and the radial surface brightness profile. Three Sérsic profiles account for the central bulge, bar, and outer disk components, respectively. We added a PSF profile to model the potential AGN component. Three stars in the image are masked. Our best-fit parameters are listed in Table 3.
Paper: Optical Continuum Reverberation Mapping of a Candidate IMBH in a Nearby Seyfert 1 Galaxy
Authors: Wenwen Zuo, Hengxiao Guo, Jingbo Sun, Qi Yuan, Paulina Lira, Minfeng Gu, Philip G. Edwards, Alok C. Gupta, Shubham Kishore, Jamie Stevens, Tao An, Zhen-Yi Cai, Hai-Cheng Feng, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, Sha-Sha Li, Mar Mezcua, Luka Č. Popović, Mouyuan Sun, Tushar Tripathi, Vivian U, Oliver Vince, Jianguo Wang, Junxian Wang, Shu Wang, Xuebing Wu, Zhenya Zheng
Figure caption: Light curves of J0249−0815 on three-night monitoring. The V-band light curve is observed by the 1.3 m DFOT in India and the ﹩{g}^{{\prime} }﹩-band light curve is from LCOGT. The single exposure time of the V band is 50 s. The photometric error in the V-band light curve is 3.6%. The filter difference (∼0.406 mag) between V and ﹩{g}^{{\prime} }﹩ is corrected based on the P200 spectrum. f  λ  is in units of 10−16 erg s−1 cm−2 Å−1.
Paper: Optical Continuum Reverberation Mapping of a Candidate IMBH in a Nearby Seyfert 1 Galaxy
Authors: Wenwen Zuo, Hengxiao Guo, Jingbo Sun, Qi Yuan, Paulina Lira, Minfeng Gu, Philip G. Edwards, Alok C. Gupta, Shubham Kishore, Jamie Stevens, Tao An, Zhen-Yi Cai, Hai-Cheng Feng, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, Sha-Sha Li, Mar Mezcua, Luka Č. Popović, Mouyuan Sun, Tushar Tripathi, Vivian U, Oliver Vince, Jianguo Wang, Junxian Wang, Shu Wang, Xuebing Wu, Zhenya Zheng
Figure caption: A gri combined image of J0249−0815 at z = 0.0297 from DECaLS with an FOV of 4′ × 4′. The positions of the target and four reference stars are denoted.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: The Compton parameter y(r ⊥) (top panel) and projected Y ⊥(r ⊥) (middle panel) reported by B+22 for their 11-galaxy stack, including their statistical error bars. The blue dashed curves are the B+22                   β-model fits to the data (Equation (32)). The green curves show our 2D PLM fit, assuming M vir = 2.75 × 1012 M ⊙, with best-fitting parameters a  P,th = 2.03, and ﹩{\phi }_{T}^{* }=2.39﹩ (see text). The bottom panel is the corner plot for the a  P,th and ﹩{\phi }_{T}^{* }﹩ posteriors. To view the data on logarithmic scales, see Figure 18 in Appendix C.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: Electron pressure (left panel) and Compton parameter profiles (middle and right panels) for the FSM models and PLM representations. In each panel, the solid curves (yellow, purple, and turquoise) are for the FSM20 isentropic (fiducial and maximal) and for the FSM17 model after the formation of the OVI component (see text). The dashed curves are the fitted PLM profiles; see Equations (11), (15), and (22). For FSM20, the PLM parameters are a  P,th = 1.64, a  n  = 0.98, and ϕ  T  = 0.71, with f hCGM = 0.29 and ﹩{\phi }_{T}^{* }=0.83﹩ for fiducial, and f hCGM = 0.59 and ﹩{\phi }_{T}^{* }=1.67﹩ for maximal. For FSM17, f hCGM = 0.77, and a  P,th = 0.78, a  n  = 0.72, and ϕ  T  = 3.05 (﹩{\phi }_{T}^{* }=10.62﹩). For all three FSM models, M vir = 1.0 × 1012 M ⊙. In drawing the PLM curves, we account for the different overdensities, Δ, of 120 and 110 assumed in FSM17 and FSM20. In Equation (11), Δ = 100.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: CGM gas fractions for all of our 648 selected TNG halos (see Figure 6). (a) Cool gas (T < 3 × 104 K); (b) intermediate temperature; (c) hot gas (T > 0.4 × T vir); and (d) total CGM gas mass. We display the medians for all halos (black curves) and the star-forming (SF), quenched (Q) halos separately (blue and red curves). The nominal PLM value f hCGM = 0.5 is the green dashed line. We also display (squares) the FSM values for f hCGM, FSM17 (turquoise), FSM20-maximal (purple), and FSM17 (yellow).
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption:  sSFR vs. M vir in the TNG100 simulation (top panel), converted to sSFR vs. the TNG100 M * estimates (middle panel), or sSFR vs. M * using the B. P. Moster et al. (2010) SMHM relation (bottom panel). The small gray dots are for the entire set of TNG100 halos at redshift z = 0. The blue and red markers are for our subset of TNG halos for which we have constructed maps and have computed Compton-y profiles. Blue diamonds are star-forming (SF) halos, with specific star formation rates sSFR > 10−11 yr−1. The red circles are quenched (Q) halos, with sSFR < 10−11 yr−1. In the middle and bottom panels, the black curves show the median sSFR for all TNG100 SF halos at redshift z = 0.