adsabs/FOCAL huggingface dataset:
The secondary eclipses of the binary are 0.03–0.04 mag deep, and so relatively small data reduction issues can have large effects on the fidelity of the light curve. Our brightness measurements were derived from aperture photometry using DAOPHOT (Stetson 1987), although we took several additional steps to increase the precision of the results. We conducted a curve-of-growth analysis of 12 apertures photometered per star using DAOGROW (Stetson 1990) in order to correct all measured stars to a uniform large aperture. We then attempted to unify the data for each filter to a consistent zero point by using ensemble photometry (Sandquist et al. 2003; Honeycutt 1992). This essentially uses all measured stars on the frame to determine magnitude offsets resulting from differences in exposure time, airmass, atmospheric transparency, and the like. Our implementation iteratively fits for position-dependent corrections that result from variations from point-spread function across the frame. These steps each brought noticeable reductions in the amount of scatter in the light curves. However, we still found that the shape of the ground-based light curves of the secondary eclipse did not match what was expected from the Kepler observations. After some investigation, we found that features in the light curve were correlated with those for the brightest star near KIC 9777062 in our images. (The star was about 70 pixels or 28″ distant on the sky, so there was no significant overlap of the point-spread function when the seeing was generally 4–8 pixels FWHM.) We found that after subtracting the light curve of this star the out-of-eclipse light levels and the shapes of the primary and secondary eclipse light curves were much more consistent from night to night. When more distant stars on the images were tested, we found a much poorer degree of correlation. We conclude that short length-scale variations were not being corrected for (and could not be corrected for, due to lack of star sampling on the image) with whole-image zero-point corrections or image-scale position-dependent corrections. The variations were of around 0.01 mag size, but could significantly affect the secondary eclipse light curves. We could not identify any features on our flat-field images that could explain the light-curve variations, and they occurred whether dome flats, twilight flats, or hybrid flats (combining the smoothed large-scale variations from the twilight flats and small-scale variations from dome flats) were used. The ground-based eclipse observations are shown in the bottom rows of Figure 1.
Citation: Honeycutt 1992
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δ Ori Aa+Ab = Mintaka Aa+Ab = 34 Ori Aa+Ab = HD 36486 A+B = BD −00 983 A+B = ALS 14 779 A+B. δ Ori is Orion’s Belt westernmost star and a multiple system at the center of the Mintaka cluster (Caballero & Solano 2008). It has two close bright visual components (Aa and Ab) and two distant dim ones (B and C) that will not be considered here. Aa is itself composed of two spectroscopic components (Aa1+Aa2) in an eclipsing orbit with a5.7325 d period, while Ab is two magnitudes fainter than the two Aa components and located 0.′′ 267 away in 1993 and moving away from the primary (Hartmann 1904; Harvin et al. 2002). We observed the system on two consecutive nights and in both cases we were able to spatially resolve Ab from Aa, this being one of the two systems in this paper (σ Ori is the other one) where the power of Lucky Spectroscopy becomes more apparent. The two spectra for Aa yield the same spectral type as for the combined Aa+Ab value from GOSSS I, O9.5 IINwk, but the lines are slightly narrower. When analyzing the data for GOSSS I, the combined spectrum was close to being (n), something that does not happen for the spatially resolved spectra (this has the additional advantage of giving us a more purespectrum for a classical O9.5 II classification standard). There are very small variations between the two epochs for Aa, likely due to the motion of Aa1 and Aa2 but the signature of the latter in the combined spectrum is very weak (Shenar et al. 2015). The two epochs for Ab yield the same spectral type, O9.7 III:(n), and in both cases there are indications of only a slight residual contamination from Aa, with the second epoch being noisier. The (n) qualifier indicates that Ab is a fast rotator, as previously noted by Harvin et al. (2002) and Shenar et al. (2015). The differences between the spectral types of Aa (Aa1+Aa2) and Ab are consistent with the Teff and log g differences measured by Shenar et al. (2015) using spectral disentangling (as opposed to the spatial deconvolution used here). Richardson et al. (2015) also spatially resolved Aa and Ab in the UV using HST/STIS and obtained very similar values of Teff around 31 kK for Aa1 and Ab, with error bars close to 2000 K, which is also consistent with our spectral classifications. That paper using UV data is the only one we have found where δ Ori Aa+Ab was spatially deconvolved, making our result the first time it has been done in the optical.
Citation: Hartmann 1904
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In Fig. 7 we compare UGC 1378’s SFR density versus gas surface density (the Schmidt–Kennicutt relation) to data in the literature. The gas surface density corresponds to H i calculated from the 0th moment map from Mishra et al. (2017) in the same areas as SFR density. Points for the HSB and LSB discs are plotted as black and grey circles, respectively. We plot the mean SFR and H i surface density for the entire galaxy with a large open circle. The black line corresponds to the relation with an exponent of 1.4 found by Kennicutt (1998). Triangles give results for LSB galaxies published by Wyder et al. (2009), and bright and faint crosses show normal spiral galaxies from Kennicutt (1998) – total and H isurface densities. A blue line shows the best-fitting relation for the H isurface density of Bluedisk galaxies from Roychowdhury et al. (2015). We also plot the SFR in the outer regions of spiral galaxies (Bigiel et al. 2010, square symbols). In Fig. 7 the UGC 1378 measurements lie between normal spirals and LSB galaxies. The HSB disc data lie above the relation plotted for normal spirals, possibly indicating that the SFR is boosted by the bar driving gas to the star-forming rings. We cannot account for molecular gas since there are no available measurements for UGC 1378. The contribution of molecular gas would likely move the HSB disc of UGC 1378 towards the locus of normal galaxies. Because the HSB SFR of UGC 1378 is close to the predicted SFR from the Kennicutt (1998) relation obtained from H i densities (faint crosses in Fig. 7). The LSB disc of UGC 1378 lies below the correlation and accounting for molecular gas would only increase the deviation from the normal Schmidt–Kennicutt relation. Similar deviations are observed in ‘classical’ LSB galaxies, Bluedisk galaxies (Roychowdhury et al. 2015), outer parts of HSB spiral galaxies (Bigiel et al. 2010), and H idiscs in early-type galaxies (Yıldız et al. 2017). These deviations for LSB galaxies are at least partially explained by their lower gas densities leading to lower SFRs (Abramova & Zasov 2011). A recent episode of gas accretion on to the disc of UGC 1378 may also contribute to a lower SFR if the gas is not yet fully participating in the star formation. Lutz et al. (2017) studied a sample of very H i rich galaxies and proposed that very high specific angular momentum in H irich galaxies prevents the accreted gas from being transported to the mid-plane of the disc and being converted into stars. This mechanism may act to preserve giant gaseous discs.
Citation: Bigiel et al. 2010
Citation function: Similarities; Similarities
Citation: Bigiel et al. 2010
Citation function: Uses; Uses
Assuming that non-jetted H ii galaxies are powered by SF, the relation between radio luminosities in such galaxies and MBH can be deciphered as a link between thermal/non-thermal SF luminosity and BH mass, in the form $L_{\rm SF} \propto M_{\rm BH}^{0.61}$, which has the largest scatter of the observed linear regressions, due to the large uncertainties of MBH estimates at low values and numerous radio non-detections. This unprecedented relation is likely the result of the observed link found between SF indicators such as radio, far-infrared, optical or line luminosities, and galaxy mass (e.g. Mauch & Sadler 2007; Gürkan et al. 2018). Moreover, the SF contribution in the radio band with respect to the AGN activity is expected to increase with galaxy mass (Aird, Coil & Georgakakis 2019). In fact, the observed correlation suggests that the radio production due to SF broadly increases with BH mass, as the latter quantity is approximately a constant proportion of the galaxy mass (from a third down to a fifth in the lowest MBH ∼ 105 M⊙, Häring & Rix 2004; Reines & Volonteri 2015; Martín-Navarro & Mezcua 2018), i.e. the stellar content: more stars likely produce more radio emission. This is consistent with the idea that SF, although mostly included in the disc (Bluck et al. 2020) and known to scale with galaxy mass (Speagle et al. 2014), would possibly also scale with MBH. More precisely, the nuclear starburst is plausibly set by the available gas mass present in the NSC (MNSC, Fernández-Ontiveros, Prieto & Acosta-Pulido 2009; Neumayer, Seth & Böker 2020), which scales with the galaxy dynamical mass ($M_{\rm NSC} \propto M _{\mathrm{ dyn}}^{0.55}$, Scott & Graham 2013), which in turn respond to the SMBH gravitational well (Cen 2015; Pitchford et al. 2016). Such a sequence of links eventually enacts the radio-MBH and radio-optical relations observed for star-forming galaxies, e.g setting the fraction of radio emission with respect to the photoionizing energy from young stellar populations and SN products.
Citation: Gürkan et al. 2018
Citation function: Uses
Pre-main-sequence stars are typically surrounded by protoplanetary disks, and since such disks are generally highly optically thick at optical/near-infrared (NIR) wavelengths, they may cast shadows on their surroundings. Such disk shadows have been observed on a wide range of angular scales; recently, high-contrast imaging has revealed shadows cast on outer disks by misaligned inner disks on subarcsecond scales (e.g., Marino et al. 2015; Benisty et al. 2018; Casassus et al. 2018). Such shadows reveal that angular distortions are common in inner disks. This is consistent with the existence of a class of self-shadowed disks in which the inner disk scale height is higher than that of the outer disk, leading to a general shadowing and related cooling of the outer disk (Dullemond & Dominik 2004; Dong 2015). A related type of disk shadow, but on a vastly larger angular scale of arcminutes, are shadows cast on large-scale reflection nebulosity. These great disk shadows can occur if a young, usually spatially unresolved, star-disk system is illuminating a reflection nebula, and are especially apparent for systems viewed close to edge-on (Hodapp et al. 2004; Pontoppidan & Dullemond 2005). Neither of these two types of disk shadow should be confused with silhouette disks that obscure background nebulosity, such as the Orion proplyds (O’dell 1998), or dark dust lanes in isolated edge-on disks (Burrows et al. 1996; Stapelfeldt et al. 1998; Duchêne et al. 2010). The projection of the disk onto a large reflection nebula can greatly magnify a small structure in the obscuring disk. Indeed, the apparent angular size of great disk shadows is only limited by the size of the reflection nebula illuminated by the central star, and may be orders of magnitude larger than the protoplanetary disk itself. Great disk shadows therefore present a unique opportunity to explore the geometry of disks on scales otherwise not resolved by direct imaging, primarily the disk scale height, inclination, and position angle.
Citation: Dullemond & Dominik 2004
Citation function: Similarities
It is also very encouraging to note that recent analyses of heavy-ion reaction experiments in terrestrial laboratories and properties of NSs from multiple messengers have led to some new progress in constraining the Esym(ρ) up to about twice the saturation density. For example, shown in Figure 1 are the values of symmetry energy at 2ρ0, that is, Esym(2ρ0), from (1) the FOPI-LAND (Russotto et al. 2011) and (2) the ASY-EOS (Russotto et al. 2016) Collaborations by analyzing the relative flows and yields of light mirror nuclei as well as neutrons and protons in heavy-ion collisions at beam energies of 400 MeV/nucleon, (3) (Chen) an extrapolation of the systematics of low-density symmetry energy (Chen 2015), (4) (Zhang & Li) direct inversions of observed NS radii, tidal deformability, and maximum mass in the high-density EOS space (Zhang et al. 2018; Zhang & Li 2019a, 2020a), (5) (Xie & Li) a Bayesian inference from the radii of canonical NSs observed by using X-rays and gravitational waves from GW170817 (Xie & Li 2019), (6) (Zhou et al.) analyses of NS radii, tidal deformability, and maximum mass within an extended Skyrme Hartree–Fock approach (eSHF) (Zhou & Chen 2019; Zhou et al. 2019), (7) (Nakazato & Suzuki) analyzing cooling timescales of protoneutron stars as well as the radius and tidal deformability of GW170817 (Nakazato & Suzuki 2019), and (8) a Bayesian inference directly from the X-ray data of seven quiescent low-mass X-ray binaries in globular clusters (Baillot d’Etivaux et al. 2019). Despite the rather different assumptions and methods used in analyzing the different types of laboratory and observational data, it is very interesting to see that they all together are consistent with a fiducial value of Esym(2ρ0) = 47 MeV within the still relatively large error bars of the individual analyses. Moreover, several recent theoretical studies also predicted values of Esym(2ρ0) consistent with its fiducial value of 47 MeV. For example, an upper bound of Esym(2ρ0) ≤ 53.2 MeV was derived recently by Tong et al. (2020) by studying the radii of neutron drops using the state-of-the-art nuclear energy density functional theories. Quantum Monte Carlo calculations using local interactions derived from chiral EFT up to next-to-next-to-leading order predicted a value of Esym(2ρ0) ≈ 46 ± 4 MeV (Lonardoni et al. 2020), while the latest many-body perturbation theory calculations with consistent nucleon-nucleon and three-nucleon interactions up to fourth order in the EFT expansion predicted a value of Esym(2ρ0) ≈ 45 ± 3 MeV (Drischler et al. 2020). They are both consistent with the fiducial value of 





 and have much smaller error bars. It is worth noting that the chiral EFT is currently applicable to a maximum density of about 2ρ0.
Citation: Zhou et al. 2019
Citation function: Uses; Uses; Uses; Similarities
To explain the morphological transformation, two main evolutionary paths have been proposed in the literature. A slow cosmological path naturally follows from the strong redshift evolution of galaxy sizes, 





 (Mosleh et al. 2012; Newman et al. 2012; van der Wel et al. 2014b; Shibuya et al. 2015). Star-forming galaxies quench star formation and add to the passive population with approximately the same size in a later epoch (van Dokkum et al. 2015; Lilly & Carollo 2016). A second, fast path involves a downward transition in the mass–size plane, at approximately constant redshift (Barro et al. 2013, 2014; Dekel & Burkert 2014; Zolotov et al. 2015). This process requires a substantial “compaction” of the formally extended star-forming galaxies. One possible mechanism would be a major merger, which is known from observations and simulations to lead to substantial angular momentum redistribution, orbit reconfiguration, and mixing (Mihos & Hernquist 1996; Wuyts et al. 2010). Another possibility is an internal angular momentum redistribution within the star-forming disk. This process has been considered to be effective at high redshift (Noguchi 1999; Immeli et al. 2004a, 2004b; Elmegreen et al. 2008; Genzel et al. 2008; Bournaud et al. 2011), when galaxies are gas rich (Tacconi et al. 2013) and effective viscous dissipation leads to radial inward transport of gas and stars with a timescale of a few hundred megayears (Dekel et al. 2009) and buildup of a central dense core (bulge component) through circumnuclear concentration of gas. Nelson et al. (2016b) find in massive galaxies at z ∼ 1.4 that central 1 kpc regions are highly attenuated by dust and are responsible for half of the total star formation rate (SFR). In conjunction with morphological quenching (Martig et al. 2009; Genzel et al. 2014a), and powerful AGN outflows (Bower et al. 2006; Croton et al. 2006; Förster Schreiber et al. 2014; Genzel et al. 2014b), the compaction process may then lead to an inside-out quenching near the Schechter mass (Tacchella et al. 2015, 2016).
Citation: Zolotov et al. 2015
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The strong linearity between the two indices shown in Figure 5 must be ascribed to their strong temperature dependence and to the proximity of the Mg ii core and FUV formation heights on one side, and Mg ii continuum and MUV on the other. Most of the radiation contributing to the FUV and MUV originates in the higher photosphere and chromosphere (Thuillier et al. 2012), where atmosphere models of quiet and magnetic structures present similar (and rather small) temperature and density gradients (c.f.r. Figure 1 in Fontenla et al. 2011). This means that, at least at first order, an increase of the activity corresponds to an increase of equal amount of the temperature and density from which both MUV and FUV, as well as Mg ii wings and core, originate. Under the assumption that the lambda-integrated fluxes can be described by a Plank function, it is easy to show that the color index must scale linearly with the temperature, at least for small temperature variations. Therefore, since the spectral brightness variations over a magnetic cycle do not exceed a few tens of K (Fontenla et al. 2011), the [FUV–MUV] color index must also scale linearly with the activity. In LTE, a linear dependence of the core/wing ratio is expected (e.g., Criscuoli et al. 2013), but such dependence is probably less obvious for the Mg ii h and k line, whose cores form in NLTE conditions. Nevertheless, collisions play an important role in the formation of the line (Linsky & Avrett 1970), making the core of this doublet strongly sensitive to temperature (e.g., Carlsson et al. 2015). Indeed, numerical magnetohydrodynamic simulations indicate that the brightness temperature derived from the Mg ii h and k cores is a good approximation for the plasma temperature at the corresponding formation heights (Leenaarts et al. 2013b). Moreover, the Bremen Mg ii index is derived from data of relatively modest spectral resolution, so that the cores are not well resolved. This means that the core intensities used to construct the Mg ii index must have a non-negligible contribution from several layers of the atmosphere, from the lower photosphere, where the response function of the spectral region between the two h and k peaks reaches its maximum (Uitenbroek 1997), to the base of the transition region (Thuillier et al. 2012; Leenaarts et al. 2013b; Carlsson et al. 2015), where the cores form. Employing again a Plank function to describe both the core and the wing intensities of the Mg ii doublet it is easy to show that the Mg ii index must scale linearly with temperature, at least for small temperature perturbations.
Citation: Criscuoli et al. 2013
Citation function: Compare/Contrast; Compare/Contrast
We use data from instruments on board STEREO-A, STEREO-B, ACE, SOHO, Wind, the Geostationary Operational Environmental Satellites (GOES), MESSENGER and the Solar Dynamics Observatory (SDO). Remote-sensing observations of the CME and the activity phenomena over the solar surface were provided by the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) instrument suite on board STEREO (Howard et al. 2008), the Large Angle and Spectrometric Coronagraph experiment (LASCO) on board SOHO (Brueckner et al. 1995), the Atmospheric Imaging Assembly (AIA; Lemen et al. 2012) on board SDO, and the X-ray telescopes on board GOES. Synoptic maps including PFSS model results provided by the Global Oscillation Network Group (GONG, http://gong.nso.edu/) and by Solarsoft PFSS package were also examined. Radio observations were provided by the S/WAVES (Bougeret et al. 2008) investigation on board STEREO and by the WAVES (Bougeret et al. 1995) experiment on board Wind. In situ energetic particle observations were provided by the Solar Electron and Proton Telescope (SEPT; MÃ¼ller-Mellin et al. 2008), the Low Energy Telescope (LET; Mewaldt et al. 2008), and the High Energy Telescope (HET; von Rosenvinge et al. 2008) on board STEREO (all of them part of the IMPACT instrument suite; Luhmann et al. 2008), the Comprehensive Suprathermal and Energetic Particle Analyzer (COSTEP; MÃ¼ller-Mellin et al. 1995), and the Energetic and Relativistic Nuclei and Electron (ERNE; Torsti et al. 1995) instrument on board SOHO, the Electron, Proton, and Alpha Monitor (EPAM; Gold et al. 1998) on board ACE, the 3D Plasma and Energetic Particle Investigation (3DP) on board Wind, and the Energetic Particle and Plasma Spectrometer (EPPS; Andrews et al. 2007) on board MESSENGER. Additionally, Fe/O ratios at ACE were obtained using data from the Solar Isotope Spectrometer (SIS; Stone et al. 1998). Finally, solar wind plasma and magnetic field data were obtained from the Plasma and Suprathermal Ion Composition (PLASTIC; Galvin et al. 2008) investigation on board STEREO, the STEREO Magnetic Field Experiment (AcuÃ±a et al. 2008), the ACE Magnetic Field Experiment (Smith et al. 1998), and the ACE/Solar Wind Electron Proton Alpha Monitor (SWEPAM; McComas et al. 1998). Due to gaps in ACE/SWEPAM data, plasma data from the Charge, Element, and Isotope Analysis System (CELIAS; Hovestadt et al. 1995) instrument on board SOHO were also used. Magnetic field data from MESSENGER were obtained from the Magnetometer Instrument on board this s/c (Anderson et al. 2007). Interplanetary disturbance identifications were cross-checked using the STEREO and ACE level 3 event list maintained by L. Jian (http://www-ssc.igpp.ucla.edu/forms/stereo/stereo_level_3.html, http://www.srl.caltech.edu/ACE/ASC/DATA/level3/) and the near-Earth ICME list maintained by I. Richardson and H. Cane (http://www.srl.caltech.edu/ACE/ASC/DATA/level3/icmetable2.htm; see also Cane & Richardson 2003).
Citation: von Rosenvinge et al. 2008
Citation function: Uses; Uses