adsabs/AstroCLIMB huggingface dataset:
Paper: First Experimental Confirmation of the CH3O + H2CO → CH3OH + HCO Reaction: Expanding the CH3OH Formation Mechanism in Interstellar Ices
Authors: Julia C. Santos, Ko-Ju Chuang, Thanja Lamberts, Gleb Fedoseev, Sergio Ioppolo, Harold Linnartz
Figure caption: Plot of the integrated area of the D2CO (ν 2 = 1679 cm−1) infrared absorption band vs. that of H2CO (ν 2 = 1727 cm−1) for three different molecule fluxes, f: 8 × 1011, 1.6 × 1012, and 3.2 × 1012 cm−2 s−1.
Paper: Insufficient Gas Accretion Caused the Decline in Cosmic Star-formation Activity Eight Billion Years Ago
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: (A) The average SFR and the average stellar mass of our sample of 11,419 galaxies. The green and red points show, respectively, the average SFRs of the subsamples of galaxies at z = 0.74–1.00 and z = 1.00–1.45, in stellar-mass bins of width 0.5 dex. The dotted lines show the star-forming main sequence of Whitaker et al. (2014), interpolated to the same redshift intervals. The average stellar mass and the average SFR of galaxies in each subsample are seen to be consistent with the star-forming main sequence. (B) The contribution of star-forming galaxies to the cosmic SFR density (see also Leslie et al. 2020). The figure shows the cosmic SFR density as a function of the stellar mass of galaxies in two redshift bins: (i) during the epoch of peak cosmic SFR density, z = 1.1–1.5 (blue), and (ii) after the epoch of peak cosmic SFR density, z = 0.8–1.1 (orange). Star-forming galaxies with M * ≥ 1010 M ⊙ (shown in the shaded region) dominate the SFR density at both epochs and contribute ≈85% to the decline in the cosmic SFR density at z ≲ 1.
Paper: Insufficient Gas Accretion Caused the Decline in Cosmic Star-formation Activity Eight Billion Years Ago
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The average HI depletion timescale, 〈tdep,HI〉≡〈M HI〉/〈SFR〉, of star-forming galaxies at z ≈ 1.1, plotted against the average stellar mass. The red circles show our measurements of the average HI depletion timescale for the two stellar-mass subsamples. The error bars along the y-axis indicate the 1σ statistical uncertainties on the measurements while the error bars along the x-axis show the 90% range of stellar masses in each subsample. The blue points show the average HI depletion timescale, 〈tdep,HI〉≡〈M HI〉/〈SFR〉, for two subsamples of xGASS galaxies at z ≈ 0 (Catinella et al. 2018), each with the same stellar-mass distribution as the corresponding DEEP2 subsample. The dashed gray line shows the H2 depletion timescale of star-forming galaxies at z ≈ 1.2 (Tacconi et al. 2013). We obtain a very short average HI depletion timescale, ≈0.86 Gyr, for star-forming galaxies with M * > 1010 M ⊙ at z ≈ 1.1, comparable to the H2 depletion timescale (Tacconi et al. 2013) in similar galaxies at z ≈ 1.2.
Paper: Insufficient Gas Accretion Caused the Decline in Cosmic Star-formation Activity Eight Billion Years Ago
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The average HI 21 cm emission and the average rest-frame 1.4 GHz continuum emission from star-forming galaxies in the two redshift subsamples. (A) The left panels show, for the two stellar-mass subsamples, the stacked HI 21 cm emission images. The circle at the bottom left of each panel shows the 90 kpc spatial resolution of the images. The contour levels are at −3.0σ (dashed), +3.0σ, +4.0σ, and +5.0σ significance. (B) The middle panels show the average HI 21 cm emission spectra; the channel width is 90 km s−1, while the dashed curves show the ±1σ error on each spectrum. The stacked HI 21 cm emission signals from both subsamples are clearly detected in both the images and the spectra. (C) The right panels show the stacked rest-frame 1.4 GHz luminosity images of the galaxies in the two subsamples. The contour levels are at 5σ, 10σ, 20σ, and 40σ statistical significance. The circle at the bottom left of each panel shows the 40 kpc resolution of the images. The average rest-frame 1.4 GHz continuum emission is clearly detected at high (>32σ) significance in both images.
Paper: Insufficient Gas Accretion Caused the Decline in Cosmic Star-formation Activity Eight Billion Years Ago
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The stacked HI 21 cm emission and the stacked rest-frame 1.4 GHz continuum emission from star-forming galaxies with different stellar masses at z ≈ 1. (A) The left panels show, for the two stellar-mass subsamples, the average HI 21 cm emission images. The circle on the bottom left of each panel shows the 90 kpc spatial resolution of the images. The contour levels are at −3.0σ (dashed), +3.0σ, +4.0σ, and +5.0σ significance. (B) The middle panels show the average HI 21 cm emission spectra for the two subsamples; the channel width is 90 km s−1, and the dashed curves show the ±1σ error on each spectrum. The average HI 21 cm emission signals from both subsamples are clearly detected in both the images and the spectra. (C) The right panels show the stacked rest-frame 1.4 GHz luminosity images of the galaxies in the two subsamples. The contour levels are at 5σ, 10σ, 20σ, 40σ, and 80σ statistical significance. The circle at the bottom left of each panel shows the 40 kpc resolution of the images. The average rest-frame 1.4 GHz continuum emission is detected at high (>37σ) significance in both images.
Paper: Insufficient Gas Accretion Caused the Decline in Cosmic Star-formation Activity Eight Billion Years Ago
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The redshift evolution of the average HI mass of star-forming galaxies over z = 0.74–1.45. The red squares show our measurements of the average HI mass of star-forming galaxies in the two redshift subsamples at 〈z〉 ≈ 1.3 and 〈z〉 ≈ 1.0, with identical stellar-mass distributions, obtained by separately stacking the HI 21 cm signals of galaxies in each subsample. The average HI mass of blue xGASS galaxies at z ≈ 0 (Catinella et al. 2018), with an identical effective stellar-mass distribution, is marked with a blue circle. The average HI mass is seen to decline steeply from z ≈ 1.3 to z ≈ 1.0, and then to decline slowly down to z ≈ 0, for galaxies of the same average stellar mass, 〈M *〉 ≈ 1010 M ⊙.
Paper: Insufficient Gas Accretion Caused the Decline in Cosmic Star-formation Activity Eight Billion Years Ago
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The redshift distributions of galaxies in the two stellar-mass subsamples. The blue histograms show the number of HI 21 cm subcubes as a function of redshift in each of the two stellar-mass subsamples; each histogram has been normalized by the total number of subcubes in its subsample. The orange histogram in each panel shows the redshift distribution of galaxies in the high stellar-mass subsample. The HI 21 cm subcubes of the lower stellar-mass subsample were assigned weights such that their effective redshift distribution is the one shown in orange, i.e., is identical to that of the higher stellar-mass subsample. The number of galaxies in each subsample is shown above each histogram, with the number of HI 21 cm subcubes in parentheses.
Paper: Insufficient Gas Accretion Caused the Decline in Cosmic Star-formation Activity Eight Billion Years Ago
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The stellar-mass distributions of galaxies in the two redshift subsamples. The blue histogram shows the number of HI 21 cm subcubes, in bins of stellar mass, in the two redshift subsamples; each histogram has been normalized by the total number of subcubes in its subsample. The orange histograms show the stellar-mass distribution of galaxies at z = 1.25–1.45. The galaxies in the lower-redshift subsample were assigned weights such that their effective stellar-mass distribution is the one shown in orange, i.e., is identical to the stellar-mass distribution of galaxies in the higher-redshift subsample. The number of galaxies in each subsample is shown above the histogram, with the number of HI 21 cm subcubes shown in parentheses.
Paper: On the Energization of Pickup Ions Downstream of the Heliospheric Termination Shock by Comparing 0.52–55 keV Observed Energetic Neutral Atom Spectra to Ones Inferred from Proton Hybrid Simulations
Authors: Matina Gkioulidou, M. Opher, M. Kornbleuth, K. Dialynas, J. Giacalone, J. D. Richardson, G. P. Zank, S. A. Fuselier, D. G. Mitchell, S. M. Krimigis, E. Roussos, I. Baliukin
Figure caption: Flux as a function of energy for SW protons (green dotted line) and PUIs (purple dotted line) averaged over nearly the entire downstream region of a hybrid model (Giacalone et al. 2021). Dashed lines represent fits of the hybrid spectra, using downstream plasma conditions in the V2 direction from the BU MHD model (Kornbleuth et al. 2021b), assuming three different populations: thermal SW protons (green), PUIs created in the supersonic SW, which are (i) adiabatically transmitted across the TS (transmitted PUIs in blue), or (ii) reflected at the TS until they have sufficient energy to overcome the cross-shock potential (energized PUIs in red). The purple solid line represents the total PUI population, combining the fits of the transmitted and energized populations.
Paper: On the Energization of Pickup Ions Downstream of the Heliospheric Termination Shock by Comparing 0.52–55 keV Observed Energetic Neutral Atom Spectra to Ones Inferred from Proton Hybrid Simulations
Authors: Matina Gkioulidou, M. Opher, M. Kornbleuth, K. Dialynas, J. Giacalone, J. D. Richardson, G. P. Zank, S. A. Fuselier, D. G. Mitchell, S. M. Krimigis, E. Roussos, I. Baliukin
Figure caption: (a) Modeled ENA fluxes, as a function of energy, calculated from simulated ion distributions using the hybrid model of Giacalone et al. (2021) (black symbols); ENA fluxes as a function of energy, as observed by IBEX-Hi (0.52–6 keV) (orange symbols) and by Cassini/INCA (5.2–55 keV) (red symbols). The observed spectra in both cases are averaged within the pixels enclosing the position of V2, over 9° for IBEX-Hi, avoiding areas in the sky that include the “ribbon”, and over 5° for INCA, from the beginning of 2009 to the end of 2012 (see the left panel of Figure 1 in Dialynas et al. 2020). The horizontal lines represent the energy range of the particular measurements, while the perpendicular lines represent the measurement uncertainties (mostly smaller than the plot symbol). (b) Ratios of observed ENA fluxes to modeled ones, as a function of energy.
Paper: Prevalence of Thermal Nonequilibrium over an Active Region
Authors: Seray Şahin, Patrick Antolin
Figure caption: (a) Composite image of a studied active region at the east limb of the Sun on 2017 June 2, co-observed by IRIS/SJI 2796 (red, dominated by the Mg II k line), IRIS/SJI 1400 (green, dominated by the Si IV 1402.77 Å line), and SDO/AIA 171 (blue, dominated by the Fe IX 171.073 Å line). The image corresponds to a variance of 30 images over intervals 08:59:54 UT and 09:16:05 UT for each channel. We applied the multiscale Gaussian normalization technique (Morgan & Druckmüller 2014) to AIA 171 Å in order to enhance the coronal structures. The yellow arrows show two legs (19 and 20, hereafter Shower 19+20) of a traced shower event, for which we study the thermodynamic evolution in Section 3.2. (b), (c), (d), (e), (f), (g), (h), and (i) composite images of some detected shower events, with their corresponding width, length, and time duration displayed on the top right of each panel. The dotted curves correspond to the shower contours based on SJI 2796.
Paper: Prevalence of Thermal Nonequilibrium over an Active Region
Authors: Seray Şahin, Patrick Antolin
Figure caption: Top: scaled emission measure (EM) plots over the white solid contour shown in Figures 3 and 4 for showers 19+20 (left) and 32 (right). The histograms correspond to the coronal rain pixels (including both legs in the case of 19+20) that are detected with the rolling Hough transform and region_grow algorithms in SJI 2796 (blue) and SJI 1400 (red). The legend identifying each curve is indicated in the top left panel (the order and colors are the same for Shower 32). Bottom: DEM-weighted temperature for both showers. The vertical black dashed lines show the start of the shower events. The vertical black dotted line indicates the time when the shower is not observed anymore at the apex. Blue dashed–dotted vertical line on Shower 19+20 plot corresponds to the time of Figures 3 and 4.
Paper: Prevalence of Thermal Nonequilibrium over an Active Region
Authors: Seray Şahin, Patrick Antolin
Figure caption: Top: time occurrence of traced shower events in SJI 2796 (a), SJI 1400 (b), and AIA 304 (c). Bottom: 1D histogram distribution of shower lengths (d), widths (e), and time durations (f), with the corresponding average and standard deviation in the inner caption. Average shower width and standard deviation with height (g).
Paper: Solar-like Dynamos and Rotational Scaling of Cycles from Star-in-a-box Simulations
Authors: Petri J. Käpylä
Figure caption: Normalized time-averaged mean angular velocity ﹩\overline{{\rm{\Omega }}}/{{\rm{\Omega }}}_{0}={\overline{U}}_{\phi }/(r\sin \theta {{\rm{\Omega }}}_{0})+1﹩ (color contours) and meridional circulation (arrows) (a), normalized kinetic helicity ﹩\tilde{{ \mathcal H }}={ \mathcal H }/({u}_{\mathrm{rms}}{\omega }_{\mathrm{rms}})﹩ (b), normalized current helicity ﹩\tilde{{ \mathcal C }}={ \mathcal C }/({u}_{\mathrm{rms}}{\omega }_{\mathrm{rms}})﹩ (c), and normalized product ﹩\widetilde{({ \mathcal H }+{ \mathcal C })\tfrac{\partial \overline{{\rm{\Omega }}}}{\partial r}}={\tau }_{\mathrm{ff}}^{3}({ \mathcal H }+{ \mathcal C })\tfrac{\partial \overline{{\rm{\Omega }}}}{\partial r}﹩ (d) from run C.
Paper: Solar-like Dynamos and Rotational Scaling of Cycles from Star-in-a-box Simulations
Authors: Petri J. Käpylä
Figure caption: Panels (a), (d), and (g): azimuthally averaged radial magnetic field ﹩{\overline{B}}_{r}(\theta ,t)﹩ from r = R for runs A (top), C (middle), and D (bottom). Panels (b), (e), and (h): azimuthally averaged toroidal field ﹩{\overline{B}}_{\phi }(\theta ,t)﹩ from r = 0.65R. The field strength is given in terms of the equipartition field B eq. Panels (c), (f), and (i): power spectra of the velocity (E K) and magnetic fields (E M) from r = 0.85R as functions of spherical harmonic degree ℓ. The gray (yellow) lines indicate nonaxisymmetric (m ≠ 0) contributions. Dotted lines indicate the Kolmogorov ℓ −5/3 scaling. The inset shows the normalized fraction of the axisymmetric (m = 0) contributions.
Paper: Neutrino Mass Bounds in the Era of Tension Cosmology
Authors: Eleonora Di Valentino, Alessandro Melchiorri
Figure caption: One-dimensional posterior distributions for Σm  ν  for several combinations of data sets under the assumption of an extended ΛCDM model (Planck analysis includes variation in the A lens parameter). A prior on the optical depth (tauprior) is present every time the ACT-DR4 and SPT-3G data are considered but neglected in the legend for brevity. The vertical dashed line identifies the value Σm  ν  = 0.26 eV, while the horizontal line is for P = 0.135, i.e., where a Gaussian distribution is at two standard deviations from the maximum. None of the posteriors exclude a value of Σm  ν  = 0.26 eV.
Paper: Neutrino Mass Bounds in the Era of Tension Cosmology
Authors: Eleonora Di Valentino, Alessandro Melchiorri
Figure caption: One-dimensional posterior distributions for Σm  ν  for several combinations of data sets under the assumption of a ΛCDM model (Planck analysis includes variation in the A lens parameter). A prior on the optical depth (tauprior) is present every time the ACT-DR4 and SPT-3G data are considered but neglected in the legend for brevity. The vertical dashed line identifies the value Σm  ν  = 0.26 eV, while the horizontal line is for P = 0.135, i.e., where a Gaussian distribution is at two standard deviations from the maximum. None of the posteriors exclude a value of Σm  ν  = 0.26 eV.
Paper: Neutrino Mass Bounds in the Era of Tension Cosmology
Authors: Eleonora Di Valentino, Alessandro Melchiorri
Figure caption: Two-dimensional contour plots for Σm  ν  vs. H 0 for the ACT-DR4 (left panel) and SPT-3G (middle panel) combinations with WMAP and the Gaussian priors on the Hubble constant R20 and F21 (a prior on the optical depth (tauprior) is present everywhere but neglected in the legend for brevity), and with the addition of BAO (right panel), under the assumption of an extended ΛCDM model.
Paper: GRB 211227A as a Peculiar Long Gamma-Ray Burst from a Compact Star Merger
Authors: Hou-Jun Lü, Hao-Yu Yuan, Ting-Feng Yi, Xiang-Gao Wang, You-Dong Hu, Yong Yuan, Jared Rice, Jian-Guo Wang, Jia-Xin Cao, De-Feng Kong, Emilio Fernandez-García, Alberto J. Castro-Tirado, Ji-Shun Lian, Wen-Pei Gan, Shan-Qin Wang, Li-Ping Xin, M. D. Caballero-García, Yu-Feng Fan, En-Wei Liang
Figure caption: Left: the follow-up observation of GRB 211227A with LCOGT, and the red circle is the location (R.A. = 08:48:35.975, decl. = −02:44:06.93) of the galaxy with a radius of 2″, and the green circle is the location (R.A. = 08:48:35.73, decl. = −02:44:07.1) of the GRB 211227A with an error radius of 2.″6. Right: distributions of the physical offsets of long and short GRBs taken from Lü et al. (2017), as well as GRB 211227A (vertical solid red line). The dashed lines are the best Gaussian fits for long and short GRBs, respectively.
Paper: GRB 211227A as a Peculiar Long Gamma-Ray Burst from a Compact Star Merger
Authors: Hou-Jun Lü, Hao-Yu Yuan, Ting-Feng Yi, Xiang-Gao Wang, You-Dong Hu, Yong Yuan, Jared Rice, Jian-Guo Wang, Jia-Xin Cao, De-Feng Kong, Emilio Fernandez-García, Alberto J. Castro-Tirado, Ji-Shun Lian, Wen-Pei Gan, Shan-Qin Wang, Li-Ping Xin, M. D. Caballero-García, Yu-Feng Fan, En-Wei Liang
Figure caption: Swift/BAT light curves of GRB 211227A in different energy bands with a 128 ms time bin (red solid lines) and the spectral evolution (red diamonds). In order to compare with GRB 060614, we also plot the light curve (black solid lines) and spectral evolution (black points) in the same panels.
Paper: GRB 211227A as a Peculiar Long Gamma-Ray Burst from a Compact Star Merger
Authors: Hou-Jun Lü, Hao-Yu Yuan, Ting-Feng Yi, Xiang-Gao Wang, You-Dong Hu, Yong Yuan, Jared Rice, Jian-Guo Wang, Jia-Xin Cao, De-Feng Kong, Emilio Fernandez-García, Alberto J. Castro-Tirado, Ji-Shun Lian, Wen-Pei Gan, Shan-Qin Wang, Li-Ping Xin, M. D. Caballero-García, Yu-Feng Fan, En-Wei Liang
Figure caption: Comparison of the observed data of the GRB 211227A from the Lijiang 2.4 m and BOOTES with those of SN 1998bw, SN 2001ke, SN 2013dx, and SN 2016jca associated with GRBs at z = 0.228 (dashed lines) and z = 1 (solid lines).
Paper: GRB 211227A as a Peculiar Long Gamma-Ray Burst from a Compact Star Merger
Authors: Hou-Jun Lü, Hao-Yu Yuan, Ting-Feng Yi, Xiang-Gao Wang, You-Dong Hu, Yong Yuan, Jared Rice, Jian-Guo Wang, Jia-Xin Cao, De-Feng Kong, Emilio Fernandez-García, Alberto J. Castro-Tirado, Ji-Shun Lian, Wen-Pei Gan, Shan-Qin Wang, Li-Ping Xin, M. D. Caballero-García, Yu-Feng Fan, En-Wei Liang
Figure caption: X-ray light curve of GRB 211227A (red diamonds). (a) Comparison with GRB 060614 (blue points), broken power-law model fits (black solid line), and the spectral evolution (insert). (b) Comparison with other short GRBs with extended emission and X-ray plateau observed by Swift from Lü et al. 2015.
Paper: GRB 211227A as a Peculiar Long Gamma-Ray Burst from a Compact Star Merger
Authors: Hou-Jun Lü, Hao-Yu Yuan, Ting-Feng Yi, Xiang-Gao Wang, You-Dong Hu, Yong Yuan, Jared Rice, Jian-Guo Wang, Jia-Xin Cao, De-Feng Kong, Emilio Fernandez-García, Alberto J. Castro-Tirado, Ji-Shun Lian, Wen-Pei Gan, Shan-Qin Wang, Li-Ping Xin, M. D. Caballero-García, Yu-Feng Fan, En-Wei Liang
Figure caption: Calculated kilonova emission of GRB 211227A at z = 0.228 by considering one energy source with M ejc ∼ 0.03 M ⊙, β ∼ 0.25c, and κ ∼ 0.97 cm2 g−1, which are taken from kilonova AT2017gfo (Yu et al. 2018).
Paper: GRB 211227A as a Peculiar Long Gamma-Ray Burst from a Compact Star Merger
Authors: Hou-Jun Lü, Hao-Yu Yuan, Ting-Feng Yi, Xiang-Gao Wang, You-Dong Hu, Yong Yuan, Jared Rice, Jian-Guo Wang, Jia-Xin Cao, De-Feng Kong, Emilio Fernandez-García, Alberto J. Castro-Tirado, Ji-Shun Lian, Wen-Pei Gan, Shan-Qin Wang, Li-Ping Xin, M. D. Caballero-García, Yu-Feng Fan, En-Wei Liang
Figure caption: Light curve of kilonova in K, R, and U bands of GRB 211227A by adopting M ejc ∼ (0.01 − 0.1) M ⊙, β ∼ 0.2c, and κ ∼ 10 cm2 g−1 at z = 0.228.
Paper: GRB 211227A as a Peculiar Long Gamma-Ray Burst from a Compact Star Merger
Authors: Hou-Jun Lü, Hao-Yu Yuan, Ting-Feng Yi, Xiang-Gao Wang, You-Dong Hu, Yong Yuan, Jared Rice, Jian-Guo Wang, Jia-Xin Cao, De-Feng Kong, Emilio Fernandez-García, Alberto J. Castro-Tirado, Ji-Shun Lian, Wen-Pei Gan, Shan-Qin Wang, Li-Ping Xin, M. D. Caballero-García, Yu-Feng Fan, En-Wei Liang
Figure caption: The spectral fits of GRB 211227A with power-law model for time-resolved (a) and (b) and time-integrated (c).
Paper: The Age of Discovery with the James Webb Space Telescope: Excavating the Spectral Signatures of the First Massive Black Holes
Authors: Kohei Inayoshi, Masafusa Onoue, Yuma Sugahara, Akio K. Inoue, Luis C. Ho
Figure caption: Color–color diagrams of the growing seed BHs at z ∼ 8 (left) and z ∼ 10 (right). We show the same objects as in Figure 3 with the same line styles. Only the colors in limited redshift ranges (6 ≤ z ≤ 10 for the F200W − F356W vs. F356W − F560W plane, and 8 ≤ z ≤ 14 for the F277W − F444W vs. F444W − F770W plane) are presented. We also show other galaxy populations: Balmer-break galaxies (orange) and extremely dusty star-forming galaxies (brown), which are obtained from the galaxy SED models used in Mawatari et al. (2020). For visualization, we overplot the colors with filled dots with an interval of Δz = 1. Galactic brown dwarfs from the BT-Settl model (Allard et al. 2012, solar-metallicity model only) are shown with magenta open symbols: M (diamond), L (circle), T (triangle), and Y (cross). O-to-M stars (magenta dot) are computed from Kurucz (1993). The color-cut conditions given in Equations (4) and (5) provide robust criteria for photometric selection of rapidly growing BHs (magenta regions). See the main text for more details.
Paper: The Age of Discovery with the James Webb Space Telescope: Excavating the Spectral Signatures of the First Massive Black Holes
Authors: Kohei Inayoshi, Masafusa Onoue, Yuma Sugahara, Akio K. Inoue, Luis C. Ho
Figure caption: Color–color diagrams for NIRCam dropout selection at z ∼ 8 (left) and z ∼ 10 (right). The colors of high-z seed BHs at 6 < z < 9 (black) are heavily contaminated by Galactic brown dwarfs (open symbols), as is also the case for Lyman-break galaxies (Hainline et al. 2020), but are clearly separated from extremely red galaxies at intermediate redshifts of z > 1.
Paper: Spatially Resolved Moving Radio Burst Associated with an EUV Wave
Authors: Lei Lu, Li Feng, Weiqun Gan
Figure caption: Physical parameters of the moving radio burst. (a) The brightness temperature at five NRH frequencies (coded by different colors) between 150 and 327 MHz. (b) Degree of circular polarization at three NRH frequencies between 150 and 228 MHz. The vertical dashed line in each panel indicates the start time of the moving radio burst. Panels (c) and (d) show the power-law fit to the NRH flux-frequency spectra at two different times, respectively. The spectral index α is shown in the upper-right corner of each panel.
Paper: Spatially Resolved Moving Radio Burst Associated with an EUV Wave
Authors: Lei Lu, Li Feng, Weiqun Gan
Figure caption: Radio dynamic spectrum from WIND/WAVES, NDA, and e-CALLISTO spectrometers, showing the solar radio bursts on 2011 September 24. The white dashed line illustrates the type IV radio burst and the black line refers to the moving radio burst under study. The inset in the bottom panel shows the time profiles of the radio emission at 150.75 MHz and the hard X-ray emission above 50 keV.