adsabs/AstroCLIMB huggingface dataset:
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: Top: a face-on view of the Galactic density distribution for detectable DCOs. We show the density distribution for the top 95% of the sources, the rest are indicated by scatter points whose sizes correspond to their sampling weights. The colored lines show the 75% contour for each of the individual DCO types. The large cross passes through (0, 0) and helps to highlight the bias toward the position of the Sun, which is indicated by the circled dot . Bottom: as Figure 3, but for the luminosity distance. </> </>
Paper: Resolving the Peak of the Black Hole Mass Spectrum
Authors: Ebraheem Farag, Mathieu Renzo, Robert Farmer, Morgan T. Chidester, F. X. Timmes
Figure caption: Normalized 3α reaction rates over core He burning temperatures 0.2–0.4 GK. Both the NACRE and JINA rates are normalized to the 3α rate from Caughlan & Fowler (1988; CF88).
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: Cumulative number of LISA detections with a given S/N. Colors indicate the LISA mission length, and the shading shows 1σ and 2σ uncertainties (obtained via bootstrapping). </>
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: The relation between dust attenuation derived from the SED fitting, E(B − V)SED, and that derived directly from the Hα/Hβ line ratio, E(B − V)Hα/Hβ . This plot shows data for CLEAR galaxies in our sample with z < 1.5 where both Hα and Hβ lines are detected. The figure shows that considering the whole sample, the nebular gas (traced by the Hα/Hβ ratio) experiences more dust attenuation than the stars (traced by the continuum, modeled by the SED fitting). A linear fit (using linmix) to the full sample shows a best fit of E(B − V)Hα/Hβ  = E(B − V)SED/(0.4 ± 0.2) (indicated by the swath of gray lines, which show random draws from the posterior of the fit). However, the majority of the galaxies ( > 66%) have E(B − V)SED < 0.13, for which the data are consistent with E(B − V)Hα/Hβ  ≈ E(B − V)SED. We therefore adopt E(B − V)nebular = E(B − V)SED, but we show in Appendix B that assuming higher dust attenuation for the nebular gas would not substantially impact any of our findings.
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Change in R 23 and O 23 emission-line ratios, and the derived gas-phase metallicity (ΔlogO/H, and ionization parameter, ﹩{Delta}\mathrm{log}q﹩) when increasing the amount of dust attenuation in the gas. Each quantity is Δx = x 2 − x 1, where x 1 is the quantity assuming equal dust attenuation in the gas and stars, and x 2 is the quantity assuming more dust attenuation in the gas (with E(B − V)nebular = E(B − V)SED/0.44). The top panels show the effects on our full sample, color-coded by E(B − V)SED. The bottom panels show medians for different subsamples (as labeled in the legends). For most of the galaxies in our sample, the increase in R 23 corresponds to a decrease in metallicity. Similarly the decrease in O 32 corresponds to a decrease in ionization parameter. However, the observed effects are small, particularly in the medians for the samples in the MZR, MQR, and when comparing the ionization parameters of the samples of “high” and “low” ionization (see the text and Section 6.4).
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: The stellar-mass, gas-phase metallicity relation (MZR) for galaxies at 1.1 < z < 1.5 from CLEAR with metallicities derived using the combination of [O II], [O III], Hβ, Hα+[N II], and [S II]. The small blue data points show the results for individual galaxies. The large data points show medians in bins of stellar mass. The shaded region shows the distribution derived using the same combination of emission lines from SDSS DR14. The black solid thin line shows our fit to the SDSS galaxies. The dotted lines show the MZR relation at z = 0.07, 0.7, and 2.2 from Maiolino et al. (2008). The histogram and curve along the top of the panel shows the distribution of stellar masses for the CLEAR galaxies in this subsample . The solid thick line shows the fit to the CLEAR galaxies in this subsample; the dashed thick line shows the fit to these same CLEAR galaxies using the metallicities derived only from [O II], [O III], and Hβ. The large circles show the relation derived by Henry et al. (2021) using all available emission lines (including data for this sample) with a different calibration of metallicity (see the text).
Paper: Evidence for the Three Wave Interactions in the Vicinity of an Interplanetary Shock
Authors: G. Thejappa
Figure caption: The electric field components of the Langmuir wave packet observed at 17.42:25.780 UT in the spacecraft frame of reference.
Paper: Evidence for the Three Wave Interactions in the Vicinity of an Interplanetary Shock
Authors: G. Thejappa
Figure caption: The electric field components of the Langmuir wave packet observed at 17:42:25.186 UT in the spacecraft frame of reference.
Paper: Evidence for the Three Wave Interactions in the Vicinity of an Interplanetary Shock
Authors: G. Thejappa
Figure caption: Top panel: the dynamic spectrum of the wave activity obtained on 2011 February 18 by the WAVES experiment of the STEREO A spacecraft from 16:00 UT to 18:00 UT in the frequency range from 10 to 38 kHz. The enhancement of the wave activity in all frequencies at 17:43:0.25 UT corresponds to a CME-driven interplanetary shock with Mach number of ∼2.32, and shock normal angle θ  Bn  ∼ 72.2°, and the extended wave activity around 25 kHz in the upstream region corresponds to Langmuir waves, excited by the shock accelerated electron beam. The location of time domain sampler (TDS) events analyzed in this study with respect to the shock is clearly indicated in the figure. Bottom panel: the time profile of the magnetic field obtained on 2011 February 18 by the STEREO A IMPACT magnetic field experiment from 16:00 UT to 18:00 UT. This clearly shows a sudden jump at 17:43:0.25 UT corresponding to the CME-driven interplanetary shock. The TDS events analyzed in this study, which occurred at 17:42:25.186 UT and 17:42:25.780 UT are shown as “*” and “+,” respectively. These wave packets show spectral peaks around 25.27 kHz and 25.20 kHz, which correspond to local electron plasma frequencies.
Paper: Evidence for the Three Wave Interactions in the Vicinity of an Interplanetary Shock
Authors: G. Thejappa
Figure caption: The fast Fourier transform spectrum of E ∥ component of the wave packet of Figure 3. Panel (a) shows the logarithmic spectrum in 10–35 kHz range, where, the peaks L and L′ probably correspond to beam-excited Langmuir waves and daughter downshifted Langmuir waves excited as a result of the three wave interaction ﹩L\to {L}^{{\prime} }+S﹩, which is called the electrostatic decay instability (ESD). The bottom panel shows the linear spectrum in the 0.65–2.0 kHz range, where the peak S probably corresponds to ion sound waves excited as a result of ESD.
Paper: The Quasar Luminosity Function at z ∼ 5 via Deep Learning and Bayesian Information Criterion
Authors: Suhyun Shin, Myungshin Im, Yongjung Kim
Figure caption: (a) Normalized histograms of the extendedness values (i − i CModel) for the HST extended (green filled) and point sources (pink hatched). The black dashed line indicates (i − i CModel) = 0.2. 98.4% of the HST point sources have (i − i CModel) < 0.2, whereas the (i − i CModel) values of the HST extended sources are almost evenly distributed. (b) The (i − i CModel) value distributions as a function of i-band magnitude for the HST extended (green squares and line) and point sources (pink circles and line). The median values of (i − i CModel) distributions are marked with squares or circles. The error bars indicate the 68% percentile of the distributions. The black dashed line indicates the extendedness value we applied to our quasar selection. (c) The fractions of the HST point and extended sources with (i − i CModel) < 0.2. The green squares indicate the point-source contamination rate caused by galaxies, and the pink circles represent the point source completeness. Although the point source contamination reaches about 40% at i < 25 mag, the completeness is always ≳90%.
Paper: Evidence for the Three Wave Interactions in the Vicinity of an Interplanetary Shock
Authors: G. Thejappa
Figure caption: The FFT spectrum of E ∥ component of the wave packet of Figure 6. The top panel shows the logarithmic spectrum in 10–35 kHz range, where, the peaks L and L′ probably correspond to beam-excited Langmuir waves and daughter downshifted Langmuir waves excited as a result of the electrostatic decay (ESD), respectively. The bottom panel shows the linear spectrum in the 0.65–2.0 kHz range, where the peak S probably corresponds to ion sound waves excited as a result of ESD.
Paper: Evidence for the Three Wave Interactions in the Vicinity of an Interplanetary Shock
Authors: G. Thejappa
Figure caption: The electric field components of the Langmuir wave packet of Figure 2 in the magnetic-field-aligned coordinate system, where E ∥ corresponds to the parallel component and E ⊥1 and E ⊥2 correspond to perpendicular components with respect to the ambient magnetic field.
Paper: Evidence for the Three Wave Interactions in the Vicinity of an Interplanetary Shock
Authors: G. Thejappa
Figure caption: The electric field components of the Langmuir wave packet of Figure 5 in the magnetic-field-aligned coordinate system, where E ∥ corresponds to the parallel component and E ⊥1 and E ⊥2 correspond to perpendicular components with respect to the ambient magnetic field.
Paper: Spatial Scales and Time Variation of Solar Subsurface Convection
Authors: Alexander V. Getling, Alexander G. Kosovichev
Figure caption: Depth variations of sample power spectra of the divergence of the velocity field smoothed with a 17.5 Mm window, p  lm , with ﹩{l}_{\max }=200,﹩ obtained by 45 day averaging over the low-activity period from 2019 December 21 to 2020 February 4. The depth values are indicated at the top of each panel.
Paper: Spatial Scales and Time Variation of Solar Subsurface Convection
Authors: Alexander V. Getling, Alexander G. Kosovichev
Figure caption: Depth variations of sample power spectra of the divergence of the unsmoothed velocity field, p  lm , with ﹩{l}_{\max }=1000﹩ obtained by 45 day averaging over the low-activity period from 2019 December 21 to 2020 February 4. The red vertical line in each spectrum marks the estimated long-wavelength spectral bound of the realization noise (Figure 3). The depth values are indicated at the top of each panel.
Paper: Spatial Scales and Time Variation of Solar Subsurface Convection
Authors: Alexander V. Getling, Alexander G. Kosovichev
Figure caption: Estimated long-wavelength bound of the realization noise for an acoustic frequency of 3 × 10−3 Hz as a function of depth.
Paper: Spatial Scales and Time Variation of Solar Subsurface Convection
Authors: Alexander V. Getling, Alexander G. Kosovichev
Figure caption: The full wavelength, λ, of the spherical harmonic Y l   m  and λ/2 for r = R ⊙, as determined by the Jeans formula (9).
Paper: Spatial Scales and Time Variation of Solar Subsurface Convection
Authors: Alexander V. Getling, Alexander G. Kosovichev
Figure caption: The same as Figure 5, but for the high-activity period from 2013 December 18 to 2014 February 1.
Paper: Spatial Scales and Time Variation of Solar Subsurface Convection
Authors: Alexander V. Getling, Alexander G. Kosovichev
Figure caption: Sample maps of the divergence field at levels d = 0.5, 4.0, 6.0, and 11.5 Mm (from left to right), at the same time.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: Fe II 5169 Å velocities of SN 2014ad evolving over time calculated using the Monte Carlo technique from Modjaz et al. (2016). SN 2014ad Fe II velocities (black) are compared to a sample of Ic (orange), Ic-bl without observed GRBs (teal), and SN-GRBs (purple). SN 2014ad consistently shows high ejecta velocities, exceeding those of typical Ic-bl, even those associated with GRBs. Note that time is given relative to V max, which for SN 2014ad occurred at ∼5.5 days after B max. Table 3 lists the Fe II velocities for SN 2014ad and their corresponding phases with respect to both B max and V max.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: Comparison between the observed UV spectrum of SN 1994I on 1994 April 19 corresponding to phase +10 days, observed UV PTF 12gzk spectrum from 2012 August 15 corresponding to phase +11 days, and the observed UV SN 2014ad spectrum from 2014 March 25 corresponding to phase +7 days. SN 1994I was smoothed and blueshifted to match PTF 12gzk and then PTF 12gzk was smoothed and blueshifted to match SN 2014ad. The smoothing is given as the FWHM of the Gaussian convolution kernel (in velocity space). The right panel is the same as the left panel but plotted on a logarithmic scale to better show the UV flux.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: Best-fit TARDIS model compared to the HST spectrum (black) for 2014 March 19 (top, blue) and 2014 March 25 (bottom, red). The 2014 March 19 model uses ﹩{t}_{\exp }=8﹩ days, v = 33,000 km s−1, and L tot = 5.0 × 1042 erg s−1. The 2014 March 25 model uses ﹩{t}_{\exp }=14﹩ days, v = 22,000 km s−1, and L tot = 4.1 × 1042 erg s−1.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: The density profile of the ejecta at +8 days postexplosion is plotted and filled in gray. A simple power-law, homologous profile is assumed, with ρ ∼ v −6. The mass fraction abundances of the elements used in our TARDIS model are overplotted. We assume uniform abundances throughout the SN ejecta. TARDIS appropriately accounts for the change in Fe-group elements as 56Ni radioactively decays over time. Element colors match those in Figure 9.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: Comparison of our TARDIS models to the TARDIS models generated using parameters from the light-curve analysis in Sahu et al. (2018) (light gray). The light-gray TARDIS model has lower density (to match the lower ejecta mass) and higher Fe-group element abundances (to match the higher 56Ni mass). The dashed light-gray model is the same as the light-gray model, but only the 56Ni abundance has been increased rather than all the Fe-group elements. In the dashed light-gray model, the Fe abundance is the same as our TARDIS models. The parameters used in our TARDIS models are given on the left, and the parameters used in the TARDIS models based on Sahu et al. (2018) are given on the right.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: Nebular spectra of SN 2014ad showing our LBT and Magellan data, along with the late-time spectrum from Sahu et al. (2018). The wavelength axis is redshift-corrected to the host-galaxy rest frame. The fluxes have been corrected for total reddening and scaled and vertically shifted for clarity. Narrow lines and telluric absorption features were manually removed and the spectra were gently smoothed; the uncorrected spectra are shown as transparent lines. Phase is given in rest-frame days relative to B maximum (MJD 56735.11; Sahu et al. 2018). Spectra are colored to match Figure 2.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: Spectral element decomposition plots for our TARDIS models of the HST spectra. These plots show the contribution of particular elements to spectral features and were generated through a visualization tool available in TARDIS.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: Similar to Figure 7, but zoomed-in to the UV wavelength range. HST data from 2014 March 19 is shown in dark blue with its corresponding TARDIS model in light blue. HST data from 2014 March 25 is shown in dark red with its corresponding TARDIS model in light red. The bottom panel is the same as the top plot, but with a log scale in luminosity. The TARDIS models are featureless and underpredict the observed flux in the UV.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption:  TARDIS models were optimized to match our HST Optical+UV data epochs (blue and red; same as in Figure 7). Here we show the model prediction compared to the data at other epochs, with the photospheric velocity as the only free parameter for each additional panel.
Paper: Walk on the Low Side: LOFAR Explores the Low-frequency Radio Emission of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Benedetta Vulcani, Bianca M. Poggianti, Alessia Moretti, Timothy Shimwell, Andrea Botteon, Reinout J. van Weeren, Ian D. Roberts, Jacopo Fritz, Neven Tomičić, Giorgia Peluso, Rosita Paladino, Myriam Gitti, Ancla Müller, Sean McGee, Marco Gullieuszik
Figure caption: (a) Diagnostic plots for JW39 (left) and JO85 (right). Top: sampling grid on top of the radio (gray) and the stellar disk (orange) contours. The star-forming cells are reported in magenta. The numbers map the points in the other panels. The black crosses show the galactic center. Center: I Rad vs. I Hα  measured from the maps in Figure 2 with the best-fit (continuous, blue for the total and orange for the disk-only) and the SFR-based (dashed, from Equation (4)) relations. Bottom: L Rad vs. SFR (SFRrecent, gold, and SFR H α , red), with the trend expected from Equation (3) (blue line). The shaded regions show the 1σ confidence interval of the best-fit relations. (b) Diagnostic plots for JO60 (left) and JW100 (right). (c) Diagnostic plots for JO49 (left) and JO206 (right).
Paper: Walk on the Low Side: LOFAR Explores the Low-frequency Radio Emission of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Benedetta Vulcani, Bianca M. Poggianti, Alessia Moretti, Timothy Shimwell, Andrea Botteon, Reinout J. van Weeren, Ian D. Roberts, Jacopo Fritz, Neven Tomičić, Giorgia Peluso, Rosita Paladino, Myriam Gitti, Ancla Müller, Sean McGee, Marco Gullieuszik
Figure caption:                         Slope k of the I                         Rad–I                         Hα                          relation for each galaxy (Figure 4). The vertical lines indicate the mean value of each distribution and the k = 1 level (dashed gray line).
Paper: Walk on the Low Side: LOFAR Explores the Low-frequency Radio Emission of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Benedetta Vulcani, Bianca M. Poggianti, Alessia Moretti, Timothy Shimwell, Andrea Botteon, Reinout J. van Weeren, Ian D. Roberts, Jacopo Fritz, Neven Tomičić, Giorgia Peluso, Rosita Paladino, Myriam Gitti, Ancla Müller, Sean McGee, Marco Gullieuszik
Figure caption: MUSE Hα images smoothed to the resolution of the corresponding LOFAR images (see Table 1) with the contours of the stellar continuum (gold dashed) and the LOFAR 144 MHz continuum emission (silver-filled contours). The radio continuum levels start from 2× the rms level (except JW100 for which they start from 3× the rms level) and progress by a factor 2.
Paper: Walk on the Low Side: LOFAR Explores the Low-frequency Radio Emission of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Benedetta Vulcani, Bianca M. Poggianti, Alessia Moretti, Timothy Shimwell, Andrea Botteon, Reinout J. van Weeren, Ian D. Roberts, Jacopo Fritz, Neven Tomičić, Giorgia Peluso, Rosita Paladino, Myriam Gitti, Ancla Müller, Sean McGee, Marco Gullieuszik
Figure caption: MUSE Hα images with the contours of the stellar continuum (gold dashed) and the LOFAR 144 MHz continuum emission (silver-filled contours). The radio continuum levels start from 2× the rms level (except JW100 for which they start from 3× the rms level) and progress by a factor 2.
Paper: Walk on the Low Side: LOFAR Explores the Low-frequency Radio Emission of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Benedetta Vulcani, Bianca M. Poggianti, Alessia Moretti, Timothy Shimwell, Andrea Botteon, Reinout J. van Weeren, Ian D. Roberts, Jacopo Fritz, Neven Tomičić, Giorgia Peluso, Rosita Paladino, Myriam Gitti, Ancla Müller, Sean McGee, Marco Gullieuszik
Figure caption: Radio luminosity at 144 MHz vs. SFR of the GASP-LOFAR (gold) and LoTSS (silver) samples. We report the empirical relations between L Rad and SFR presented by Gürkan et al. (2018) (blue) and Roberts et al. (2021b) (red), the latter is fitted to the LoTSS sample. The shaded regions show the dispersion at 1σ around the corresponding best-fit relations.