adsabs/AstroCLIMB huggingface dataset:
Paper: Nonstop Variability of Sgr A* Using JWST at 2.1 and 4.8 μm Wavelengths: Evidence for Distinct Populations of Faint and Bright Variable Emission
Authors: F. Yusef-Zadeh, H. Bushouse, R. G. Arendt, M. Wardle, J. M. Michail, C. J. Chandler
Figure caption: Same as Figure 7 but showing day 4 data.
Paper: Monster Radio Jet (>66 kpc) Observed in Quasar at z  ∼​​​​​ 5
Authors: Anniek J. Gloudemans, Frits Sweijen, Leah K. Morabito, Emanuele Paolo Farina, Kenneth J. Duncan, Yuichi Harikane, Huub J. A. Röttgering, Aayush Saxena, Jan-Torge Schindler
Figure caption: Left: LOFAR VLBI image of the extended radio jet of J1601+3102 at 144 MHz superimposed on an optical z-band image of the DESI Legacy Imaging Survey. The radio contours are drawn at [−1, 1, 2, 4, 8, 16, 32] × 3σrms with σrms = 0.08 mJy beam−1. The beam size (resolution of 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩3) is shown in the bottom left corner. The source shows a northern and a southern lobe at a distance of 1﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩4 and 8﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩9 from the optical quasar, which equals a projected distance of 9 and 57 kpc, respectively. The physical size of the extended radio jet is therefore >66 kpc, making this the largest radio jet at z > 4 to date. Top right: low-resolution 50″ radio cutouts from LoTSS, FIRST, and VLASS with radio contours drawn at [−1, 0.5, 1, 2, 4, 8, 16, 32] × 3σrms. The respective beam sizes are indicated in the bottom left corner. The white rectangle corresponds to the LOFAR VLBI image in the left panel, and the red crosses indicate the position of the optical quasar. Bottom right: radio spectrum from 144 MHz to 3 GHz derived from these three radio surveys. The northern lobe is detected in all surveys; however, the southern lobe is only detected in LoTSS and FIRST. The nondetection in VLASS is given as a 3σ upper limit. The spectra are well described by a power law with the scatter indicated by the dashed lines. The spectral indices derived from these surveys are nearly identical with ﹩-1.2{6}_{-0.06}^{+0.06}﹩ and ﹩-1.2{7}_{-0.10}^{+0.13}﹩ for the northern and southern lobe, respectively.
Paper: Monster Radio Jet (>66 kpc) Observed in Quasar at z  ∼​​​​​ 5
Authors: Anniek J. Gloudemans, Frits Sweijen, Leah K. Morabito, Emanuele Paolo Farina, Kenneth J. Duncan, Yuichi Harikane, Huub J. A. Röttgering, Aayush Saxena, Jan-Torge Schindler
Figure caption: Physical properties of J1601+3102 compared to the literature. Left: black hole mass of J1601+3102 derived from the Mg II line vs. the bolometric luminosity compared to other known high-z quasars from E. P. Farina et al. (2022). The contours highlight the distribution of SDSS DR16 quasars in the range 0.27 < z < 2.72 from Q. Wu & Y. Shen (2022). The systematic error on the black hole mass of ∼​​​​​0.55 dex is shown in the bottom right corner. The SMBH mass of J1601+3102 is lower than the average of this population, whereas the Eddington ratio is similar. Right: projected jet size of J1601+3102 compared to known high-redshift radio galaxies (A. Saxena et al. 2019) and quasars (J0309+2717, C. Spingola et al. 2020; P172+18, E. Momjian et al. 2021; J0131–0321/J1146+4037, Y. Shao et al. 2022). J1601+3102 is the first quasar at z > 4 with a large resolved radio jet.
Paper: The Extraordinary Long-lasting Infrared Echo of PS16dtm Reveals an Extremely Energetic Nuclear Outburst
Authors: Ning Jiang, Di Luo, Jiazheng Zhu, Roc M. Cutri
Figure caption: The multiwavelength light curves for PS16dtm. The Swift/UVOT photometry is denoted by square in different colors, the ZTF and ATLAS photometry by dots, and the WISE photometry by triangles. The red dashed line shows the estimated Gaussian-fitted rise of PS16dtm using both ASAS-SN-V and Swift-V (tpeak = 57677 ± 5, σrise = 58 ± 2). The black dashed line shows the estimated power-law decay fitted decline of PS16dtm using ATLAS o-band with an index of −1.66 ± 0.06. All magnitudes are in the AB magnitude system, except for WISE, which uses the Vega magnitude system.
Paper: Monster Radio Jet (>66 kpc) Observed in Quasar at z  ∼​​​​​ 5
Authors: Anniek J. Gloudemans, Frits Sweijen, Leah K. Morabito, Emanuele Paolo Farina, Kenneth J. Duncan, Yuichi Harikane, Huub J. A. Röttgering, Aayush Saxena, Jan-Torge Schindler
Figure caption: Top panel: composite optical and infrared spectrum of J1601+3102 obtained with HET/LRS2 (<8500 Å) and Gemini/GNIRS (>8500  Å) binned to a resolution of 200 km s−1. The error of the GNIRS spectrum (gray) increases significantly toward bluer wavelengths. The continuum is described by a power law + iron pseudocontinuum (purple line; see Section 2.4). The wavelength regions heavily affected by telluric lines are masked for visualization purposes. The inset shows the Mg II line including the best fit with an FWHM of 2694﹩{}_{-383}^{+510}﹩ km s−1. Bottom panel: the residual flux divided by the error spectrum after subtracting the continuum and Lyα, N V, C IV, C III], and Mg II emission line fits (see Appendix B.1). The gray shaded regions show the masked regions for continuum fitting.
Paper: Monster Radio Jet (>66 kpc) Observed in Quasar at z  ∼​​​​​ 5
Authors: Anniek J. Gloudemans, Frits Sweijen, Leah K. Morabito, Emanuele Paolo Farina, Kenneth J. Duncan, Yuichi Harikane, Huub J. A. Röttgering, Aayush Saxena, Jan-Torge Schindler
Figure caption: The fitted spectrum (dashed line) of the delay calibrator ILT J155955.03+304223.7, based on the photometry available in NED (squares) and the flux density as measured from the channel images output by WSClean (circles).
Paper: Monster Radio Jet (>66 kpc) Observed in Quasar at z  ∼​​​​​ 5
Authors: Anniek J. Gloudemans, Frits Sweijen, Leah K. Morabito, Emanuele Paolo Farina, Kenneth J. Duncan, Yuichi Harikane, Huub J. A. Röttgering, Aayush Saxena, Jan-Torge Schindler
Figure caption: Zoom-in on the Lyα and N V emission lines (left), C IV line (middle), and C III] line (right). The spectrum is fitted using a power law and iron continuum (purple) and single Gaussian emission lines (yellow). The noise spectrum is indicated in gray.
Paper: Nonstop Variability of Sgr A* Using JWST at 2.1 and 4.8 μm Wavelengths: Evidence for Distinct Populations of Faint and Bright Variable Emission
Authors: F. Yusef-Zadeh, H. Bushouse, R. G. Arendt, M. Wardle, J. M. Michail, C. J. Chandler
Figure caption: Same as Figure 7 but showing day 7 data.
Paper: Nonstop Variability of Sgr A* Using JWST at 2.1 and 4.8 μm Wavelengths: Evidence for Distinct Populations of Faint and Bright Variable Emission
Authors: F. Yusef-Zadeh, H. Bushouse, R. G. Arendt, M. Wardle, J. M. Michail, C. J. Chandler
Figure caption: Similar to Figure 9 (left two columns) except that more complex flares with multiple subflares are selected.
Paper: Nonstop Variability of Sgr A* Using JWST at 2.1 and 4.8 μm Wavelengths: Evidence for Distinct Populations of Faint and Bright Variable Emission
Authors: F. Yusef-Zadeh, H. Bushouse, R. G. Arendt, M. Wardle, J. M. Michail, C. J. Chandler
Figure caption: Same as Figure 7 but showing day 6 data.
Paper: Nonstop Variability of Sgr A* Using JWST at 2.1 and 4.8 μm Wavelengths: Evidence for Distinct Populations of Faint and Bright Variable Emission
Authors: F. Yusef-Zadeh, H. Bushouse, R. G. Arendt, M. Wardle, J. M. Michail, C. J. Chandler
Figure caption: Same as Figure 7 but showing day 5 data.
Paper: Nonstop Variability of Sgr A* Using JWST at 2.1 and 4.8 μm Wavelengths: Evidence for Distinct Populations of Faint and Bright Variable Emission
Authors: F. Yusef-Zadeh, H. Bushouse, R. G. Arendt, M. Wardle, J. M. Michail, C. J. Chandler
Figure caption: Left: four panels show light curves of Sgr A* by connecting the data points and are constructed, days 1–4, of observations in 2023. Blue and red dots correspond to 2.1 and 4.8 μm, respectively. The sampling time is 46 and 25 s on days 1–3 and day 4, respectively (see Table 1). Correlated variability is detected. Extinction corrections have been applied. The extinction correction increases the measured 2.1 and 4.8 μm flux densities by factors of 11.16 and 3.94, respectively. Linear fits to the changing pedestal have been made in all epochs at 2.1 (blue) and 4.8 (red) μm. To estimate the pedestal, the solid lines are fourth-degree polynomial fits to the data. The differing curves indicate that the pedestal varies in brightness and spectral index. There is a tendency to be relatively redder when flaring is brighter, but this could be an artifact of the estimated background level that has been subtracted from all Sgr A* photometry. Note that the F480M filter was not available on day 3. These figures show the evidence for long-term variability of the quiescent emission (pedestal) from Sgr A*. Right: similar to the left panels except that the light curves of days 5–7 in 2024 are displayed. The sampling time is 18.2 s in days 5–7 in 2024. Correlated variability in both the F210M and F480M bands is detected. The 1σ error bars at 2.1 and 4.8 μm are 0.0015 and 0.03 mJy, respectively, and are too small to display.
Paper: Nonstop Variability of Sgr A* Using JWST at 2.1 and 4.8 μm Wavelengths: Evidence for Distinct Populations of Faint and Bright Variable Emission
Authors: F. Yusef-Zadeh, H. Bushouse, R. G. Arendt, M. Wardle, J. M. Michail, C. J. Chandler
Figure caption: Extinction-corrected light curves of Sgr A* and reference stars for all 7 days concatenated together at 2.1 and 4.8 μm are presented in linear and logarithmic scales in the top and bottom panels, respectively. The light curves of the reference stars S0-17 and “Ref,” a random nearby star in the field with a similar signal level as Sgr A*, are displayed in the top panel as black and gray points, respectively. The reference stars are stable, whereas Sgr A* is always fluctuating. Vertical dashed lines separate 7 different noncontiguous days. These plots indicate that the observed variations in Sgr A* at both wavelengths are real and not an artifact or noise. In addition, the amplitude of the quiescent flux of Sgr A* and pedestal emission vary on daily, monthly, and yearly timescales.
Paper: The Extraordinary Long-lasting Infrared Echo of PS16dtm Reveals an Extremely Energetic Nuclear Outburst
Authors: Ning Jiang, Di Luo, Jiazheng Zhu, Roc M. Cutri
Figure caption: The single power-law (left panel; f = Aλ−n) and blackbody (right panel) fits to the SED of PS16dtm around its optical peak (MJD ∼ 57730.5, +72 days). The fitting incorporates a free parameter for dust extinction, modeled similarly to that observed in the SMC. In each panel, the best-fit SED is represented by a blue line, while the orange dots denote the observed photometry at the peak epoch. The power-law fit yields a very steep slope (index n = 6.5) and a χ2 value of 10.9, compared with an AGN-like SED (index fixed at n = 1.5) fitting result with χ2 of 141.2, and the blackbody fit gives a very high temperature (6.5 × 105 K) yet with a much worse χ2 value of 47.7. It is worth noting that the strong extinction from the SMC introduces some of the bumps and wiggles observed in the otherwise smooth model.
Paper: Nonstop Variability of Sgr A* Using JWST at 2.1 and 4.8 μm Wavelengths: Evidence for Distinct Populations of Faint and Bright Variable Emission
Authors: F. Yusef-Zadeh, H. Bushouse, R. G. Arendt, M. Wardle, J. M. Michail, C. J. Chandler
Figure caption: Astrometrically corrected NIRCam 2.1 μm (top) and 4.8 μm (middle) and ALMA 230 GHz (bottom) images of the Galactic center region. These images were simultaneously taken on 2023 September 22 and are astrometrically aligned with each other. Images on the left are zoomed out to show the locations of the well-known members of the stellar cluster, such as S0-2, orbiting Sgr A*, as well as the unidentified reference star (“Ref”) used to compare to Sgr A*. Images on the right are zoomed in to show the immediate vicinity of Sgr A* along with the comparison star S0-17. White pixels in the NIRCam images are completely saturated and have no usable signal values.
Paper: The Extraordinary Long-lasting Infrared Echo of PS16dtm Reveals an Extremely Energetic Nuclear Outburst
Authors: Ning Jiang, Di Luo, Jiazheng Zhu, Roc M. Cutri
Figure caption: The distribution of dust echo model parameters for PS16dtm. The unit of Rdust,i and Rdust,f is light year. The red dashed lines denote the location of maximum likelihood, corresponding to the parameter values of λ = 87.7, ϵΩϵdust = 0.0056, Rdust,i = 1.10 pc, and Rdust,f = 1.59 pc. The values and errors above the plots correspond to the 15.87%, 50%, and 84.13% quantile values of the posterior samples of the parameters, and the black dashed lines show the locations of these values in the plots. The contours in the 2D contour plots reflect the relative numerical density, where darker color means a larger numerical density.
Paper: The Extraordinary Long-lasting Infrared Echo of PS16dtm Reveals an Extremely Energetic Nuclear Outburst
Authors: Ning Jiang, Di Luo, Jiazheng Zhu, Roc M. Cutri
Figure caption: The dust temperature (top panel) and luminosity (bottom panel) evolution of PS16dtm. In the bottom panel, the black and blue dots denote the dust IR luminosity and OUV luminosity, respectively. The red dashed line corresponds to the rising phase of the OUV light curve, which is fitted with a Gaussian function. This phase is poorly sampled by observations but is essential for our model.
Paper: The Extraordinary Long-lasting Infrared Echo of PS16dtm Reveals an Extremely Energetic Nuclear Outburst
Authors: Ning Jiang, Di Luo, Jiazheng Zhu, Roc M. Cutri
Figure caption: Schematic picture of the dust echo model. The central SMBH, accretion disk, and dusty torus are shown in black, blue, and orange, respectively. The gray region represents the evaporated part after the outburst of PS16dtm. We have also marked the physical scale at the bottom to show the evaporation area of the torus. Note that the scale does not apply to the BH and accretion disk, which are otherwise too small to visualize.
Paper: The Extraordinary Long-lasting Infrared Echo of PS16dtm Reveals an Extremely Energetic Nuclear Outburst
Authors: Ning Jiang, Di Luo, Jiazheng Zhu, Roc M. Cutri
Figure caption: The best-fitting IR luminosity light curve. The red error bars denote the real IR luminosity estimated from blackbody fit of WISE data, while the blue curve denotes the simulated IR light curve. The shaded blue area shows the 3σ uncertainty of the simulated light curve.
Paper: Discovery of Local Analogs to JWST’s Little Red Dots
Authors: Ruqiu Lin, Zhen-Ya Zheng, Chunyan Jiang, Fang-Ting Yuan, Luis C. Ho, Junxian Wang, Linhua Jiang, James E. Rhoads, Sangeeta Malhotra, L. Felipe Barrientos, Isak Wold, Leopoldo Infante, Shuairu Zhu, Xiang Ji, Xiaodan Fu
Figure caption: Left column: comparison of rest-frame UV-to-optical SEDs between the V-shaped BLGPs at z ∼ 0.3 (green dots) and an LRD (JADES 10013704) at z = 5.9 reported in R. Maiolino et al. (2024; red dots). The green circles represent the continuum flux after subtracting emission lines. The background red line and the image in the upper left are the NIRSpec/PRISM spectrum and the NIRCam F115W-F200W-F444W color cutout of JADES 10013704. The green line is the SDSS spectra for each V-shaped BLGP, rebinned to the spectral resolution of NIRSpec/PRISM resolution. All photometries and spectra are normalized at rest-frame 5800 Å. For each V-shaped BLGP, the SDSS gri color cutout is also illustrated in the upper right of the corresponding subfigure. The observing dates of the image and spectra for each V-shaped BLGP are also labeled. Right column: emission-line measurement for the V-shaped BLGPs. The black, blue, and green lines are the observed spectra, the narrow (or wide) components, and the composite spectra. The green shade is the broad Hα component.
Paper: Discovery of Local Analogs to JWST’s Little Red Dots
Authors: Ruqiu Lin, Zhen-Ya Zheng, Chunyan Jiang, Fang-Ting Yuan, Luis C. Ho, Junxian Wang, Linhua Jiang, James E. Rhoads, Sangeeta Malhotra, L. Felipe Barrientos, Isak Wold, Leopoldo Infante, Shuairu Zhu, Xiang Ji, Xiaodan Fu
Figure caption: Panel (a): optical continuum slope vs. BH mass for BLGPs (stars). For comparison, we illustrate high-z broad-line AGNs including LRDs reported in R. Maiolino et al. (2024), J. Matthee et al. (2023), J. E. Greene et al. (2024), and Y. Harikane et al. (2023), if available. Panel (b): BPT diagram. The classification lines follow L. J. Kewley et al. (2001; solid line) and G. Kauffmann et al. (2003; dashed line), also seen in L. J. Kewley et al. (2006). Here, we also mark JADES 10013704 in big diamonds. Panel (c): bolometric luminosity vs. BH mass. The gray lines indicate Eddington ratios of λEdd =  1, 0.1, 0.01.
Paper: Discovery of Local Analogs to JWST’s Little Red Dots
Authors: Ruqiu Lin, Zhen-Ya Zheng, Chunyan Jiang, Fang-Ting Yuan, Luis C. Ho, Junxian Wang, Linhua Jiang, James E. Rhoads, Sangeeta Malhotra, L. Felipe Barrientos, Isak Wold, Leopoldo Infante, Shuairu Zhu, Xiang Ji, Xiaodan Fu
Figure caption: MBH vs. M* diagram. For comparison, we illustrate high-z broad-line AGNs including LRDs reported in R. Maiolino et al. (2024), D. D. Kocevski et al. (2023), and Y. Harikane et al. (2023). Six LRDs with stellar mass measurements derived by C.-H. Chen et al. (2024) are also plotted. The black dashed lines illustrate the local MBH–M* relations derived for all, early-type, and late-type galaxies (J. E. Greene et al. 2020). The solid line represents the scaling relation for AGNs evolved to z  = 0 (M.-Y. Zhuang & L. C. Ho 2023). The dotted line represents the MBH–M* relation at 4 < z < 7 (F. Pacucci et al. 2023). Shaded areas show 1σ intrinsic scatters.
Paper: Discovery of Local Analogs to JWST’s Little Red Dots
Authors: Ruqiu Lin, Zhen-Ya Zheng, Chunyan Jiang, Fang-Ting Yuan, Luis C. Ho, Junxian Wang, Linhua Jiang, James E. Rhoads, Sangeeta Malhotra, L. Felipe Barrientos, Isak Wold, Leopoldo Infante, Shuairu Zhu, Xiang Ji, Xiaodan Fu
Figure caption: Optical continuum slope βopt vs. UV continuum slope βUV for the GPs hosting broad-line AGNs (stars). The shaded area presents the LRD selection criteria (D. D. Kocevski et al. 2024) with the V-shaped UV-to-optical SEDs. The V-shaped BLGPs are marked on blue squares. The color bar shows the fraction of broad to total Hα flux for our BLGP sample. For comparison, we illustrate high-z broad-line AGNs including LRDs reported in J. Matthee et al. (2023) and J. E. Greene et al. (2024).
Paper: On the Abiotic Origin of Dimethyl Sulfide: Discovery of Dimethyl Sulfide in the Interstellar Medium
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Christian P. Endres, Valerio Lattanzi, Izaskun Jiménez-Serra, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, David San Andrés, Belén Tercero, Pablo de Vicente, Sergio Martín, Miguel A. Requena-Torres, Paola Caselli, Jesús Martín-Pintado
Figure caption: (a) Selected transitions of DMS identified toward the GC molecular cloud G+0.693-0.027, which were used to derive the LTE physical parameters of the molecule (see text; listed in Table 1). (b) Additional transitions of DMS observed in the astronomical data set that further support the detection but were excluded from the fit because of a nonnegligible line blending with either known species or U-lines (listed in Table B1; see Figures B1 and B2 for the rest of the observed lines). The red lines show the best LTE fit of DMS, while the blue lines represent the combined emission of all molecules identified in the survey, including DMS (observed spectra are shown as black histograms with gray shaded areas). The transitions are sorted by increasing frequency. The structure of DMS, optimized at the B2PLYPD3/aug-cc-pVTZ level using Gaussian 16 (M. J. Frisch et al. 2016), is also shown (carbon atoms in gray, sulfur atom in yellow, and hydrogen atoms in white).
Paper: On the Abiotic Origin of Dimethyl Sulfide: Discovery of Dimethyl Sulfide in the Interstellar Medium
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Christian P. Endres, Valerio Lattanzi, Izaskun Jiménez-Serra, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, David San Andrés, Belén Tercero, Pablo de Vicente, Sergio Martín, Miguel A. Requena-Torres, Paola Caselli, Jesús Martín-Pintado
Figure caption: All the transitions of DMS observed toward the GC molecular cloud G+0.693-0.027 above an integrated S/N of ​​​​​​∼3, which include those used to derive the LTE physical parameters of the molecule highlighted with a yellow star (see main text; listed in Table 1) together with many other transitions, marked with a green star, that are consistent with the observations but were excluded from the fit because of a nonnegligible line blending with either known species or U-lines, or due to a lower S/N ratio. The result of the best LTE fit of DMS is plotted with a red line, and the blue line depicts the emission from all the molecules identified to date in the survey, including DMS (observed spectra shown as gray histograms and light gray shaded areas). The transitions are sorted by increasing frequency.
Paper: On the Abiotic Origin of Dimethyl Sulfide: Discovery of Dimethyl Sulfide in the Interstellar Medium
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Christian P. Endres, Valerio Lattanzi, Izaskun Jiménez-Serra, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, David San Andrés, Belén Tercero, Pablo de Vicente, Sergio Martín, Miguel A. Requena-Torres, Paola Caselli, Jesús Martín-Pintado
Figure caption: Rotational diagram of DMS toward G+0.693 (blue dots, including 1σ errors). The best linear fit to the data points is shown using a gray dotted line. The derived values for the molecular column density, N, and the excitation temperature, Tex, are shown in blue.
Paper: On the Abiotic Origin of Dimethyl Sulfide: Discovery of Dimethyl Sulfide in the Interstellar Medium
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Christian P. Endres, Valerio Lattanzi, Izaskun Jiménez-Serra, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, David San Andrés, Belén Tercero, Pablo de Vicente, Sergio Martín, Miguel A. Requena-Torres, Paola Caselli, Jesús Martín-Pintado
Figure caption: Same as in Figure B1 but for additional lines.
Paper: The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster
Authors: Xiang-Lei Chen, Chao-Wei Tsai, Di Li, Pei Wang, Yi Feng, Jun-Shuo Zhang, Guo-Dong Li, Yong-Kun Zhang, Lu-Lu Bao, Mai Liao, Lu-Dan Zhang, Pei Zuo, Dong-Wei Bao, Chen-Hui Niu, Rui Luo, Wei-Wei Zhu, Hu Zou, Sui-Jian Xue, Bing Zhang
Figure caption: SFR and stellar mass of FRB host galaxies. The host galaxy of FRB 20240114A, other dwarf host galaxies, and the host galaxy of the active repeater FRB 20201124A are highlighted with larger symbols outlined in black, with their names labeled near the symbols. The unfilled red star represents the SFR(radio) of the host galaxy of FRB 20201124A (Y. Dong et al. 2024). The dashed gray line indicates the SFMS at redshift z = 0.1. The dotted purple lines denote equal-sSFR levels of sSFR = 10−9,10−10, and 10−11. The contours represent SDSS galaxies (DR7; K. N. Abazajian et al. 2009) with redshifts between 0.01 and 0.2, provided by the MPA-JHU catalog.
Paper: The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster
Authors: Xiang-Lei Chen, Chao-Wei Tsai, Di Li, Pei Wang, Yi Feng, Jun-Shuo Zhang, Guo-Dong Li, Yong-Kun Zhang, Lu-Lu Bao, Mai Liao, Lu-Dan Zhang, Pei Zuo, Dong-Wei Bao, Chen-Hui Niu, Rui Luo, Wei-Wei Zhu, Hu Zou, Sui-Jian Xue, Bing Zhang
Figure caption: BPT classification diagram for the host galaxy of FRB 20240114A and that of other FRBs. The contours represent the SDSS DR17 galaxies with significant emission lines (>5σ, Abdurro’uf et al. 2022). The lines indicate the demarcation between star-forming galaxies and composite sources (G. Kauffmann et al. 2003a), composite sources and LINERs (L. J. Kewley et al. 2006), and LINER and Seyfert galaxies (R. Cid Fernandes et al. 2010), respectively.