adsabs/AstroCLIMB huggingface dataset:
Paper: Accretion from Winds of Red Giant Branch Stars May Reveal the Supermassive Black Hole in Leo I
Authors: Fabio Pacucci, Abraham Loeb
Figure caption: Detectability analysis of the peak microwave emission of Leo I* by ALMA in band 10 (∼850 GHz, ∼1.1 mJy continuum sensitivity). The parameter space includes mass-loss rates and the fraction of gas accreted from RGB stars within the Bondi radius of Leo I*. The source is undetected at 1.1 mJy continuum sensitivity below the dashed line.
Paper: Accretion from Winds of Red Giant Branch Stars May Reveal the Supermassive Black Hole in Leo I
Authors: Fabio Pacucci, Abraham Loeb
Figure caption: Spectral energy distributions for the SMBH Leo I*, computed for 10 values of the Eddington ratio, equally spaced logarithmically between 9 × 10−8 and 9 × 10−7. Continuum sensitivities for the Very Large Array (VLA), Atacama Large Millimeter/submillimeter Array (ALMA), and Chandra are displayed. For the VLA, we consider its 6 GHz band and an observation time of 10 minutes. For ALMA, we consider its 850 GHz band (band 10) and an integration time of 1 minute. For Chandra, we assume photon energy of 6 keV and an integration time of 35 ks, obtaining ∼10 photons.
Paper: Laboratory and Astronomical Detection of the SiP Radical (X2Π i ): More Circumstellar Phosphorus
Authors: L. A. Koelemay, M. A. Burton, A. P. Singh, P. M. Sheridan, J. J. Bernal, L. M. Ziurys
Figure caption: Spectra of SiP (X2Πi) measured toward IRC+10216 using the ARO telescopes. The temperature scale is T A*(K). The positions of the four phosphorus hyperfine components are given in red (or gray scale) underneath each spectrum. In the top panel, the J = 8.5 → 7.5 transition is shown near 135 GHz, which appears as a shoulder on the J = 48.5 → 47.5 transition of C6H. The two middle panels display the J = 13.5 → 12.5 and J = 16.5 → 15.5 lines near 215 and 263 GHz, respectively, which are uncontaminated and display a broadened linewidth due to hyperfine structure. The bottom panel shows the J = 17.5 → 16.5 transition near 279 GHz, which appears in between two stronger features arising from Si13CC and SiC2 (v3 = 1). The ESCAPADE fits are shown over the line profiles in the inset in each panel. The spectra at 1 mm were measured with the ARO SMT (2 MHz resolution), while the 2 mm line was observed with the ARO 12 m (1.25 MHz resolution). Integration times are 103, 112, 113, and 61 hr for 215 GHz, 262 GHz, 278 GHz, and 135 GHz.
Paper: Laboratory and Astronomical Detection of the SiP Radical (X2Π i ): More Circumstellar Phosphorus
Authors: L. A. Koelemay, M. A. Burton, A. P. Singh, P. M. Sheridan, J. J. Bernal, L. M. Ziurys
Figure caption: Laboratory spectra of SiP (X2Πi) in the Ω = 3/2 ladder showing the J = 30.5 ← 29.5, J = 14.5 ← 13.5 and J = 9.5 ← 8.5 rotational transitions near 485 GHz, 231 GHz, and 151 GHz, respectively. The lambda doublets are labeled by e and f , and the phosphorus hyperfine components by quantum number F (F  f  and F  e  specifically). The J = 30.5 ← 29.5 line (top panel) only shows lambda doublets, as the hyperfine is collapsed. In the J = 14.5 ← 13.5 transition (middle panel), the spectrum is a doublet of doublets, as the hyperfine interaction is resolved. For the J = 9.5 ← 8.5 line (lower panel), the hyperfine components of opposite lambda doublets blend together, creating doublets with broader linewidths. The spectrum in the top panel is a single 110 MHz wide scan, truncated to 30 MHz; the middle and lower spectra are six scan averages, each 10 MHz in frequency.
Paper: An Electron-scattering Time Delay in Black Hole Accretion Disks
Authors: Greg Salvesen
Figure caption: Left/black axis: thermalization time delay t th in milliseconds, as a function of disk radius in gravitational units. Parameter choices are deliberately suggestive, but represent an XRB in the intermediate state (l d = 0.2) with a BH mass m = 10 and BH spin a * = 0 (solid), 0.9 (dashed), 0.998 (dotted). We set α = 0.2, ρ */ρ = 0.1, β = 0.5, l c = 0.05, h c = 10. Right/red axis: light-travel time delay t lt for a face-on observer (i = 0°). Thin vertical lines mark the narrow annulus where t th > t lt for the a * = 0.9 case. Inset: for a representative low/hard state (l d = 0.02), t th is negligible.
Paper: A Segmented Period–Luminosity Relation for Nearby Extragalactic Delta Scuti Stars
Authors: C. E. Martínez-Vázquez, R. Salinas, A. K. Vivas, M. Catelan
Figure caption: Period vs. absolute magnitude in V plane of δ Sct  stars in different environments. Top left: the LMC. Top right: the SMC. For guidance, background gray dots represent the δ Sct  stars from the LMC (combined OGLE + SuperMACHO sample). Bottom left: dSph galaxies. For guidance, background gray dots represent the δ Sct  stars from the LMC and the SMC. Bottom right: Galactic (field and globular clusters) δ Sct  stars. Background gray dots are the combined δ Sct  samples from the LMC, the SMC, and dSph galaxies. See the main text for references for each sample.
Paper: A Segmented Period–Luminosity Relation for Nearby Extragalactic Delta Scuti Stars
Authors: C. E. Martínez-Vázquez, R. Salinas, A. K. Vivas, M. Catelan
Figure caption: Density map of the δ Sct  stars in the period vs. absolute magnitude in V plane. The top left panel shows the fit obtained in this work while the rest of the panels show a comparison between this new fit and previous PLR available in the literature. References: N94 (Nemec et al. 1994), M11 (McNamara 2011), CS12 (Cohen & Sarajedini 2012), F15 (Fiorentino et al. 2015), Z19 (Ziaali et al. 2019), J20 (Jayasinghe et al. 2020).
Paper: An Electron-scattering Time Delay in Black Hole Accretion Disks
Authors: Greg Salvesen
Figure caption: Total thermal radiative flux ﹩{F}_{{\rm{r}}}^{* }﹩ at the effective photosphere (left axis) and the corresponding effective temperature ﹩{T}_{\mathrm{eff}}^{* }﹩ (right axis), as a function of disk radius. Parameter choices are the same as in Figure 2, and for BH spin a * = 0 (solid), 0.9 (dashed), 0.998 (dotted). Thin horizontal lines mark the energy band of the thermal flux emitted from the narrow annulus where t th > t lt for the a * = 0.9 case.
Paper: An Electron-scattering Time Delay in Black Hole Accretion Disks
Authors: Greg Salvesen
Figure caption: Thermalization time delay t th relative to the light-travel time delay t lt (i = 0°), as a function of disk radius. Changing one parameter in the a * = 0.9 reference model of Figure 2 (black dashed) isolates its effect on t th/t lt: no relativistic corrections (red), ζ = 2 (green), ξ = 2 (blue), f = 0.05 (brown), l c = 0.1 (purple), and m = 109 (orange).
Paper: A Segmented Period–Luminosity Relation for Nearby Extragalactic Delta Scuti Stars
Authors: C. E. Martínez-Vázquez, R. Salinas, A. K. Vivas, M. Catelan
Figure caption:  VR vs. V for the stars in common between OGLE and SuperMACHO. The black line shows the fit to the data. Only stars represented with blue filled circles have been used in the fit, while stars shown as open red crosses have been rejected by an iterative 2.5σ clipping algorithm.
Paper: An Electron-scattering Time Delay in Black Hole Accretion Disks
Authors: Greg Salvesen
Figure caption: Reverberation lags are time delays between changes in the direct coronal emission and the corresponding variations in the disk-reprocessed emission. At the long-duration limit of our proposed scattering time delay is the thermalization time delay t th, which is the time taken by the scattering random walk during the thermalization process within the disk atmosphere.
Paper: Detecting the Oscillation and Propagation of the Nascent Dynamic Solar Wind Structure at 2.6 Solar Radii Using Very Long Baseline Interferometry Radio Telescopes
Authors: Maoli Ma, Guifré Molera Calvés, Giuseppe Cimò, Ming Xiong, Peijia Li, Jing Kong, Peijin Zhang, Jiansen He, Lijia Liu, Pradyumna Kummamuru, Chuanpeng Hou, Jasper Edwards, Qinghui Liu, Zhong Chen, Zhanghu Chu, De Wu, Xu Zhao, Zhichao Wang, Songtao Han, Quanquan Zhi, Yingkai Liu, Jonathan Quick, Javier González, Cristina García Miró, Mikhail Kharinov, Andrey Mikhailov, Alexander Neidhardt, Tiziana Venturi, Marco Morsiani, Giuseppe Maccaferri, Bo Xia, Hua Zhang, Longfei Hao
Figure caption: The frequency fluctuation (FF) and the carrier-to-noise ratio (CNR) of Tianwen-1 (TIW) (a) and MEX (b) from individual telescopes. The FF is shifted by a constant value given in the legend. The CME entered the LASCO-C2 field of view at 07:09. The CME front arrived the projected Mars position around 07:20. The effects of the CME on the signal weaken after 07:32 and fade away after 11:00. In (a), the frequency jumps appear at 08:37:16 and 08:51:12; only at Mc are the radio frequency interferences (RFIs). In (b), an RFI appears at the same time 08:07:23 from Hh, Zc, Bd, Ys, and Mc stations when observing MEX.
Paper: Detecting the Oscillation and Propagation of the Nascent Dynamic Solar Wind Structure at 2.6 Solar Radii Using Very Long Baseline Interferometry Radio Telescopes
Authors: Maoli Ma, Guifré Molera Calvés, Giuseppe Cimò, Ming Xiong, Peijia Li, Jing Kong, Peijin Zhang, Jiansen He, Lijia Liu, Pradyumna Kummamuru, Chuanpeng Hou, Jasper Edwards, Qinghui Liu, Zhong Chen, Zhanghu Chu, De Wu, Xu Zhao, Zhichao Wang, Songtao Han, Quanquan Zhi, Yingkai Liu, Jonathan Quick, Javier González, Cristina García Miró, Mikhail Kharinov, Andrey Mikhailov, Alexander Neidhardt, Tiziana Venturi, Marco Morsiani, Giuseppe Maccaferri, Bo Xia, Hua Zhang, Longfei Hao
Figure caption: The spikes in frequency fluctuations at different moments from individual telescopes. ((I), (II), (III), and (IV)). Spikes among Hh, Bd, and Zc from TIW. (V) Spikes among Yg from Mars Express (MEX), Hh, Bd, Zc from TIW. ((VI)–(VII)). Spikes among Hh, Zc, Ys, and Mc from TIW. (VIII) Spikes from Hh, Zc, and Mc from TIW.
Paper: Detecting the Oscillation and Propagation of the Nascent Dynamic Solar Wind Structure at 2.6 Solar Radii Using Very Long Baseline Interferometry Radio Telescopes
Authors: Maoli Ma, Guifré Molera Calvés, Giuseppe Cimò, Ming Xiong, Peijia Li, Jing Kong, Peijin Zhang, Jiansen He, Lijia Liu, Pradyumna Kummamuru, Chuanpeng Hou, Jasper Edwards, Qinghui Liu, Zhong Chen, Zhanghu Chu, De Wu, Xu Zhao, Zhichao Wang, Songtao Han, Quanquan Zhi, Yingkai Liu, Jonathan Quick, Javier González, Cristina García Miró, Mikhail Kharinov, Andrey Mikhailov, Alexander Neidhardt, Tiziana Venturi, Marco Morsiani, Giuseppe Maccaferri, Bo Xia, Hua Zhang, Longfei Hao
Figure caption: The cross-correlation function of frequency fluctuations of Hh-Ys (a), Hh-Mc (b), and Hh-Zc (c). (I) 10:00–10:30. (II) 10:30–11:00. (III) 11:00–11:30. (IV) 11:30–12:00. (V) 12:00–12:30. (VI) 12:30–13:00.
Paper: Detecting the Oscillation and Propagation of the Nascent Dynamic Solar Wind Structure at 2.6 Solar Radii Using Very Long Baseline Interferometry Radio Telescopes
Authors: Maoli Ma, Guifré Molera Calvés, Giuseppe Cimò, Ming Xiong, Peijia Li, Jing Kong, Peijin Zhang, Jiansen He, Lijia Liu, Pradyumna Kummamuru, Chuanpeng Hou, Jasper Edwards, Qinghui Liu, Zhong Chen, Zhanghu Chu, De Wu, Xu Zhao, Zhichao Wang, Songtao Han, Quanquan Zhi, Yingkai Liu, Jonathan Quick, Javier González, Cristina García Miró, Mikhail Kharinov, Andrey Mikhailov, Alexander Neidhardt, Tiziana Venturi, Marco Morsiani, Giuseppe Maccaferri, Bo Xia, Hua Zhang, Longfei Hao
Figure caption: The correlation coefficient, lag, and velocity of the solar wind. The circle plots with Ys-Hh and Mc-Hh relate to the “fast stream.” ((I), (II), and (III)) The CC, lag, and velocity along the radial direction. ((IV), (V), and (VI)) The CC, lag, and velocity along the tangential direction.
Paper: Detecting the Oscillation and Propagation of the Nascent Dynamic Solar Wind Structure at 2.6 Solar Radii Using Very Long Baseline Interferometry Radio Telescopes
Authors: Maoli Ma, Guifré Molera Calvés, Giuseppe Cimò, Ming Xiong, Peijia Li, Jing Kong, Peijin Zhang, Jiansen He, Lijia Liu, Pradyumna Kummamuru, Chuanpeng Hou, Jasper Edwards, Qinghui Liu, Zhong Chen, Zhanghu Chu, De Wu, Xu Zhao, Zhichao Wang, Songtao Han, Quanquan Zhi, Yingkai Liu, Jonathan Quick, Javier González, Cristina García Miró, Mikhail Kharinov, Andrey Mikhailov, Alexander Neidhardt, Tiziana Venturi, Marco Morsiani, Giuseppe Maccaferri, Bo Xia, Hua Zhang, Longfei Hao
Figure caption: Power density spectra (PSD) of Mars Express (MEX) and Tianwen-1 (TIW) at Ys station at 08:30 on October 9. (I) MEX. (II) TIW and the dynamic signal model. The main carrier of TIW is obscured by the noise. (III) Recovering of the signal of TIW with local correlation.
Paper: Detecting the Oscillation and Propagation of the Nascent Dynamic Solar Wind Structure at 2.6 Solar Radii Using Very Long Baseline Interferometry Radio Telescopes
Authors: Maoli Ma, Guifré Molera Calvés, Giuseppe Cimò, Ming Xiong, Peijia Li, Jing Kong, Peijin Zhang, Jiansen He, Lijia Liu, Pradyumna Kummamuru, Chuanpeng Hou, Jasper Edwards, Qinghui Liu, Zhong Chen, Zhanghu Chu, De Wu, Xu Zhao, Zhichao Wang, Songtao Han, Quanquan Zhi, Yingkai Liu, Jonathan Quick, Javier González, Cristina García Miró, Mikhail Kharinov, Andrey Mikhailov, Alexander Neidhardt, Tiziana Venturi, Marco Morsiani, Giuseppe Maccaferri, Bo Xia, Hua Zhang, Longfei Hao
Figure caption: The LASCO pictures. (I) The CME entered the LASCO-C2 field of view at 07:09. ((II)–(III)) The CME front arrived at the projected Mars position. (IV) The CME weakens after 08:00. ((V)–(VI)). The fade away of the CME.
Paper: Detecting the Oscillation and Propagation of the Nascent Dynamic Solar Wind Structure at 2.6 Solar Radii Using Very Long Baseline Interferometry Radio Telescopes
Authors: Maoli Ma, Guifré Molera Calvés, Giuseppe Cimò, Ming Xiong, Peijia Li, Jing Kong, Peijin Zhang, Jiansen He, Lijia Liu, Pradyumna Kummamuru, Chuanpeng Hou, Jasper Edwards, Qinghui Liu, Zhong Chen, Zhanghu Chu, De Wu, Xu Zhao, Zhichao Wang, Songtao Han, Quanquan Zhi, Yingkai Liu, Jonathan Quick, Javier González, Cristina García Miró, Mikhail Kharinov, Andrey Mikhailov, Alexander Neidhardt, Tiziana Venturi, Marco Morsiani, Giuseppe Maccaferri, Bo Xia, Hua Zhang, Longfei Hao
Figure caption: The velocity obtained from the visual spikes and the cross correlation. (I) Radial velocity. (II) Tangential velocity.
Paper: Nanoflare Heating of the Solar Corona Observed in X-Rays
Authors: Vishal Upendran, Durgesh Tripathi, N. P. S. Mithun, Santosh Vadawale, Anil Bhardwaj
Figure caption: Comparison of the observed light curve from XSM (orange), and the PSM forward model of best-fit parameters inferred from our inversion code (black) in 1–2.3 keV energy band from 2019 (subfigure: I) and 2020 (subfigure: II). Each subfigure has four panels depicting the following. Panel (a): observed and simulated light curves. Panel (b): distribution of observed and simulated light-curve intensities. Panel (c): global Morlét power for observation and simulations, with the uncertainties presented in orange and blue bands. Panel (d): comparison of simulation and observation intensity CDF. The inset reports the inferred parameter set for the respective data.
Paper: Nanoflare Heating of the Solar Corona Observed in X-Rays
Authors: Vishal Upendran, Durgesh Tripathi, N. P. S. Mithun, Santosh Vadawale, Anil Bhardwaj
Figure caption: Flow chart detailing the various steps in our algorithm. First, the iPSM is trained on simulations. Next, the trained model is used to infer p  f , τ, and α. Finally, the y max and y min are inferred by minimizing an error metric.
Paper: Nanoflare Heating of the Solar Corona Observed in X-Rays
Authors: Vishal Upendran, Durgesh Tripathi, N. P. S. Mithun, Santosh Vadawale, Anil Bhardwaj
Figure caption: The XSM observed light curves considered in this work. The left (right) column is for 2019 (2020) observations. Top row is the light curve for 1.0–1.3 keV, middle row is for 1.3–2.3 keV and the bottom row is for 1.0–2.3 keV.
Paper: Nanoflare Heating of the Solar Corona Observed in X-Rays
Authors: Vishal Upendran, Durgesh Tripathi, N. P. S. Mithun, Santosh Vadawale, Anil Bhardwaj
Figure caption: The variation of metric with y max (x-axis) and y min(y-axis). The two parameters are presented here in code units (note the log scale), while the metric is presented in scale of log10. The blue circle shows the originally selected y max and y min (as used by the iPSM), while the green star corresponds to be combination with lowest metric value.
Paper: Nanoflare Heating of the Solar Corona Observed in X-Rays
Authors: Vishal Upendran, Durgesh Tripathi, N. P. S. Mithun, Santosh Vadawale, Anil Bhardwaj
Figure caption: Frequency distribution of impulsive events inferred from the observations in year 2019 (pink) and 2020 (cyan). The scatter is frequency distribution of event energies from the model. The error bars on inferred parameters are obtained by propagating the Monte Carlo uncertainties. The black scatter shows the inferred frequency distribution from Vadawale et al. (2021b), while the black dotted–dashed line corresponds to α = 2.0.
Paper: Nanoflare Heating of the Solar Corona Observed in X-Rays
Authors: Vishal Upendran, Durgesh Tripathi, N. P. S. Mithun, Santosh Vadawale, Anil Bhardwaj
Figure caption: Same as Figure 4, but for 1.3–2.3 keV band for the segment from year 2020.
Paper: Nanoflare Heating of the Solar Corona Observed in X-Rays
Authors: Vishal Upendran, Durgesh Tripathi, N. P. S. Mithun, Santosh Vadawale, Anil Bhardwaj
Figure caption: Same as Figure 4, but for 1.3–2.3 keV band.
Paper: Monochromatic Globular Clusters as a Critical Test of Formation Models for the Dark Matter–deficient Galaxies NGC 1052-DF2 and NGC 1052-DF4
Authors: Pieter van Dokkum, Zili Shen, Aaron J. Romanowsky, Roberto Abraham, Charlie Conroy, Shany Danieli, Dhruba Dutta Chowdhury, Michael A. Keim, J. M. Diederik Kruijssen, Joel Leja, Sebastian Trujillo-Gomez
Figure caption: Top panels: images of DF2 and DF4 in the HST/ACS I 814 filter, after applying flat-field corrections to the flc files and drizzling. The images span 80″ × 80″. Bottom panels: photometry procedure for two of the globular clusters, indicated with yellow boxes above. From left to right, we show the original I 814 image (with a size of 7″ × 7″), the final object mask, the PSF-convolved King (1962) model fit with the best-fitting background plane, and the cleaned image. The cleaned image is the original image with the masked areas filled in by the King model. Colors and total magnitudes are measured from aperture photometry on the cleaned V 606 and I 814 images.
Paper: Monochromatic Globular Clusters as a Critical Test of Formation Models for the Dark Matter–deficient Galaxies NGC 1052-DF2 and NGC 1052-DF4
Authors: Pieter van Dokkum, Zili Shen, Aaron J. Romanowsky, Roberto Abraham, Charlie Conroy, Shany Danieli, Dhruba Dutta Chowdhury, Michael A. Keim, J. M. Diederik Kruijssen, Joel Leja, Sebastian Trujillo-Gomez
Figure caption: Top panel: DF2/DF4 globular clusters in the color–magnitude plane. Solid symbols are spectroscopically confirmed, and light-colored symbols have uncertainties <0.015 mag. The parameterized distribution for globular clusters in low-luminosity Virgo galaxies is shown in gray (see text). Bottom-left panel: mean color of globular clusters with uncertainties <0.015, compared to Virgo galaxies from Peng et al. (2006). There is no significant systematic color difference between DF2 and DF4. Bottom-right panel: observed and intrinsic scatter in the colors, again compared to Virgo galaxies. The clusters in DF2 and DF4 are extremely homogeneous. The orange line is the minimum possible scatter, arising from stochastic fluctuations in the number of red giants.
Paper: Monochromatic Globular Clusters as a Critical Test of Formation Models for the Dark Matter–deficient Galaxies NGC 1052-DF2 and NGC 1052-DF4
Authors: Pieter van Dokkum, Zili Shen, Aaron J. Romanowsky, Roberto Abraham, Charlie Conroy, Shany Danieli, Dhruba Dutta Chowdhury, Michael A. Keim, J. M. Diederik Kruijssen, Joel Leja, Sebastian Trujillo-Gomez
Figure caption: Top-left panel: zoom-in on color–magnitude measurements with errors <0.015, corresponding to all clusters with M 606 < −8.6. Error bars are the measurement uncertainty (black), the combined measurement and flat-fielding uncertainty (dark gray), and the combined measurement, flat-fielding, and stochastic sampling uncertainty (light gray). Dotted orange lines show the expected ±1σ variation due to stochastic sampling alone. Solid lines include the other uncertainties. Top-right panel: likelihood for the intrinsic dispersion, for the photometric errors (broken line), and for the total error, including the effect of stochastic sampling (solid line). Bottom: the effects of stochastic sampling of the isochrone. Intrinsic cluster-to-cluster color differences of 0.01–0.02 mag arise from random variations in the number of red giants. Two examples of identical clusters with different random seeds are shown on the left (see the text for details).
Paper: The HI Mass Function of Star-forming Galaxies at z ∼ 0.35
Authors: Apurba Bera, Nissim Kanekar, Jayaram N. Chengalur, Jasjeet S. Bagla
Figure caption: The M H I–M  B  relation for blue galaxies at z ∼ 0.35: The solid blue circles show our estimates of ﹩\langle \mathrm{log}({{\rm{M}}}_{{\rm{H}}\,{\rm\small{I}}})\rangle ﹩ values in blue galaxies in the three M  B  bins at z ≈ 0.35 plotted against the median M  B  values. The error bars are estimated by jackknife resampling. The horizontal error bars show the bin widths. The solid black line shows the best-fit M H I–M  B  scaling relation at z ≈ 0.35, while the blue shaded region shows the 68% confidence interval around the scaling relation. The red dashed line indicates the M H I–M  B  relation at z ≈ 0 (Dénes et al. 2014).
Paper: Monochromatic Globular Clusters as a Critical Test of Formation Models for the Dark Matter–deficient Galaxies NGC 1052-DF2 and NGC 1052-DF4
Authors: Pieter van Dokkum, Zili Shen, Aaron J. Romanowsky, Roberto Abraham, Charlie Conroy, Shany Danieli, Dhruba Dutta Chowdhury, Michael A. Keim, J. M. Diederik Kruijssen, Joel Leja, Sebastian Trujillo-Gomez
Figure caption: Color images of the galaxies, created by dividing binned and median-filtered I 814 and V 606 images of the galaxies. Numerical values are simply the ratios of the observed fluxes in e− s−1. The mean value for the globular clusters is indicated with the circle. Color variations within each galaxy are caused by surface brightness fluctuations. The average color of DF4 is slightly redder than that of DF2 but the difference is not significant: ﹩{({V}_{606}-{I}_{814})}_{\mathrm{DF}2}=0.420\pm 0.024﹩ and ﹩{({V}_{606}-{I}_{814})}_{\mathrm{DF}4}=0.436\pm 0.075﹩. The galaxies are redder than the globular clusters.
Paper: The HI Mass Function of Star-forming Galaxies at z ∼ 0.35
Authors: Apurba Bera, Nissim Kanekar, Jayaram N. Chengalur, Jasjeet S. Bagla
Figure caption: The stacked HI 21 cm emission spectra (in luminosity density) for blue galaxies in the three M  B  bins, [A] − 16.0 ≥ M  B  > − 17.6, [B] −17.6 ≥ M  B  > −19.2, and [C] − 19.2 ≥ M  B  ≥ − 22.0. The dashed black curves in each panel show the rms noise in the corresponding velocity planes of the stacked spectral cubes. See text for details.