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10.1016/j.newar.2024.101694 | Subsequently, Andrews et al. (2017) selected a wide binary candidate sample from TGAS with an emphasis on purity, using a Bayesian method to calculate the probability that a given pair of stars is gravitationally bound. | Subsequently, selected a wide binary candidate sample from TGAS with an emphasis on purity, using a Bayesian method to calculate the probability that a given pair of stars is gravitationally bound. | 58 | [
"10.1093/mnras/stx2000"
] | 20,240,601 | [
"2017MNRAS.472..675A"
] | Subsequently, [REF] selected a wide binary candidate sample from TGAS with an emphasis on purity, using a Bayesian method to calculate the probability that a given pair of stars is gravitationally bound. |
10.1016/j.newar.2024.101694 | Andrews et al. (2017) investigated how the separation of their candidate pairs varied with distance and astrometric uncertainties. | investigated how the separation of their candidate pairs varied with distance and astrometric uncertainties. | 61 | [
"10.1093/mnras/stx2000"
] | 20,240,601 | [
"2017MNRAS.472..675A"
] | [REF] investigated how the separation of their candidate pairs varied with distance and astrometric uncertainties. |
10.1016/j.newar.2024.101694 | This led Andrews et al. (2017) to conclude that most of the pairs with separations 1 0 5 au reported in other works were chance alignments, not gravitationally bound binaries. | This led to conclude that most of the pairs with separations 1 0 5 au reported in other works were chance alignments, not gravitationally bound binaries. | 64 | [
"10.1093/mnras/stx2000"
] | 20,240,601 | [
"2017MNRAS.472..675A"
] | This led [REF] to conclude that most of the pairs with separations 1 0 5 au reported in other works were chance alignments, not gravitationally bound binaries. |
10.1016/j.newar.2024.101694 | It may also owe in part to the mass ratio distribution adopted in population synthesis models, which is more top-heavy than observed (e.g. El-Badry et al., 2019 ). | It may also owe in part to the mass ratio distribution adopted in population synthesis models, which is more top-heavy than observed (e.g. ). | 90 | [
"10.1093/mnras/stz2480"
] | 20,240,601 | [
"2019MNRAS.489.5822E"
] | It may also owe in part to the mass ratio distribution adopted in population synthesis models, which is more top-heavy than observed (e.g. [REF] ). |
10.1016/j.newar.2024.101694 | Hwang et al. (2022c) used a related method to study the eccentricity distribution of a larger sample of 1 0 5 wide binaries within 200 pc from Gaia DR3. | used a related method to study the eccentricity distribution of a larger sample of 1 0 5 wide binaries within 200 pc from Gaia DR3. | 110 | [
"10.3847/2041-8213/ac7c70"
] | 20,240,601 | [
"2022ApJ...933L..32H"
] | [REF] used a related method to study the eccentricity distribution of a larger sample of 1 0 5 wide binaries within 200 pc from Gaia DR3. |
10.1016/j.newar.2024.101694 | Hwang et al. (2022c) inferred an eccentricity distribution consistent with uniform at separations of 100 au , and steadily increasing eccentricities over 100 1000 au ( Fig. 3 , bottom right). | inferred an eccentricity distribution consistent with uniform at separations of 100 au , and steadily increasing eccentricities over 100 1000 au ( Fig. 3 , bottom right). | 115 | [
"10.3847/2041-8213/ac7c70"
] | 20,240,601 | [
"2022ApJ...933L..32H"
] | [REF] inferred an eccentricity distribution consistent with uniform at separations of 100 au , and steadily increasing eccentricities over 100 1000 au ( Fig. 3 , bottom right). |
10.1016/j.newar.2024.101694 | 3.1.5 The mass ratio distribution and twin binaries The homogeneity and well-understood selection function of the Gaia data allowed El-Badry et al. (2019) to infer the intrinsic mass ratio distribution of wide binaries as a function of primary mass and separation. | 3.1.5 The mass ratio distribution and twin binaries The homogeneity and well-understood selection function of the Gaia data allowed to infer the intrinsic mass ratio distribution of wide binaries as a function of primary mass and separation. | 122 | [
"10.1093/mnras/stz2480"
] | 20,240,601 | [
"2019MNRAS.489.5822E"
] | 3.1.5 The mass ratio distribution and twin binaries The homogeneity and well-understood selection function of the Gaia data allowed [REF] to infer the intrinsic mass ratio distribution of wide binaries as a function of primary mass and separation. |
10.1016/j.newar.2024.101694 | Hwang et al. (2022) showed that the eccentricities of the wide twins are on average higher than those of non-twins with similar separations. | showed that the eccentricities of the wide twins are on average higher than those of non-twins with similar separations. | 130 | [
"10.3847/2041-8213/ac7c70"
] | 20,240,601 | [
"2022ApJ...933L..32H"
] | [REF] showed that the eccentricities of the wide twins are on average higher than those of non-twins with similar separations. |
10.1016/j.newar.2024.101694 | El-Badry and Rix (2019) attempted to constrain the separation below which metallicity dependence appears using a sample of wide binaries from Gaia DR2 and metallicities from several wide-field surveys. | attempted to constrain the separation below which metallicity dependence appears using a sample of wide binaries from Gaia DR2 and metallicities from several wide-field surveys. | 140 | [
"10.1093/mnras/stz2480"
] | 20,240,601 | [
"2019MNRAS.489.5822E"
] | [REF] attempted to constrain the separation below which metallicity dependence appears using a sample of wide binaries from Gaia DR2 and metallicities from several wide-field surveys. |
10.1016/j.newar.2024.101694 | Hwang et al. (2021) and Hwang et al. (2022b) focused on wide binaries ( 1000 au) and found more complicated behavior than the flat trend with metallicity reported by El-Badry and Rix (2019) : they found that the wide binary fraction peaks at [ Fe/H ] = 0 and declines towards both higher and lower metallicities. | and focused on wide binaries ( 1000 au) and found more complicated behavior than the flat trend with metallicity reported by : they found that the wide binary fraction peaks at [ Fe/H ] = 0 and declines towards both higher and lower metallicities. | 143 | [
"10.1093/mnras/staa3854",
"10.3847/2041-8213/ac7c70",
"10.1093/mnras/stz2480"
] | 20,240,601 | [
"2021MNRAS.501.4329H",
"2022ApJ...933L..32H",
"2019MNRAS.489.5822E"
] | [REF] and [REF] focused on wide binaries ( 1000 au) and found more complicated behavior than the flat trend with metallicity reported by [REF] : they found that the wide binary fraction peaks at [ Fe/H ] = 0 and declines towards both higher and lower metallicities. |
10.1016/j.newar.2024.101694 | Curiously, comparison of their sample and the sample used by El-Badry and Rix (2019) suggested that the discrepant results are in large part due to different treatments of hierarchical triples: El-Badry and Rix (2019) employed cuts on relative proper motion that excluded most triples, while Hwang et al. (2022b) include... | Curiously, comparison of their sample and the sample used by suggested that the discrepant results are in large part due to different treatments of hierarchical triples: employed cuts on relative proper motion that excluded most triples, while included them, and the triples seem to cluster at [ Fe/H ] = 0 . | 144 | [
"10.1093/mnras/stz2480",
"10.3847/2041-8213/ac7c70"
] | 20,240,601 | [
"2019MNRAS.489.5822E",
"2022ApJ...933L..32H"
] | Curiously, comparison of their sample and the sample used by [REF] suggested that the discrepant results are in large part due to different treatments of hierarchical triples: [REF] employed cuts on relative proper motion that excluded most triples, while [REF] included them, and the triples seem to cluster at [ Fe/H ]... |
10.1016/j.newar.2024.101694 | Triples can thus be identified as wide binaries in which the apparent velocity difference between the two resolved components is larger than expected for a bound orbit, but still smaller than expected for chance alignments (e.g. El-Badry et al., 2021 ). | Triples can thus be identified as wide binaries in which the apparent velocity difference between the two resolved components is larger than expected for a bound orbit, but still smaller than expected for chance alignments (e.g. ). | 177 | [
"10.1093/mnras/stab323"
] | 20,240,601 | [
"2021MNRAS.506.2269E"
] | Triples can thus be identified as wide binaries in which the apparent velocity difference between the two resolved components is larger than expected for a bound orbit, but still smaller than expected for chance alignments (e.g. [REF] ). |
10.1016/j.newar.2024.101694 | In his now-seminal study using adaptive optics imaging of nearby spectroscopic binaries, Tokovinin et al. (2006) found that 96 7 % of solar-type binaries with P 3 d have a wide companion. | In his now-seminal study using adaptive optics imaging of nearby spectroscopic binaries, found that 96 7 % of solar-type binaries with P 3 d have a wide companion. | 191 | [
"10.1051/0004-6361:20054427"
] | 20,240,601 | [
"2006A&A...450..681T"
] | In his now-seminal study using adaptive optics imaging of nearby spectroscopic binaries, [REF] found that 96 7 % of solar-type binaries with P 3 d have a wide companion. |
10.1016/j.newar.2024.101694 | 3.3 Tests of gravity Binaries with separations larger than 1 0 4 au have sufficiently low internal accelerations that they are in the so-called deep MOND regime: that is, the Modified Newtonian Dynamics (MOND; Milgrom, 1983 ) theory of gravity predicts measurably different orbital velocities from general relativity. | 3.3 Tests of gravity Binaries with separations larger than 1 0 4 au have sufficiently low internal accelerations that they are in the so-called deep MOND regime: that is, the Modified Newtonian Dynamics (MOND; ) theory of gravity predicts measurably different orbital velocities from general relativity. | 197 | [
"10.1086/161130"
] | 20,240,601 | [
"1983ApJ...270..365M"
] | 3.3 Tests of gravity Binaries with separations larger than 1 0 4 au have sufficiently low internal accelerations that they are in the so-called deep MOND regime: that is, the Modified Newtonian Dynamics (MOND; [REF] ) theory of gravity predicts measurably different orbital velocities from general relativity. |
10.1016/j.newar.2024.101694 | Projection effects tend to increase the apparent velocity difference of wide binaries ( El-Badry, 2019 ). | Projection effects tend to increase the apparent velocity difference of wide binaries ( ). | 204 | [
"10.1093/mnras/stz2480"
] | 20,240,601 | [
"2019MNRAS.489.5822E"
] | Projection effects tend to increase the apparent velocity difference of wide binaries ( [REF] ). |
10.1016/j.newar.2024.101694 | In another study, Banik et al. (2024) found Newtonian gravity to be strongly preferred ( 16 ) over MOND, with relatively weak sensitivity to the assumed eccentricity distribution and parameters of the inner binary population. | In another study, found Newtonian gravity to be strongly preferred ( 16 ) over MOND, with relatively weak sensitivity to the assumed eccentricity distribution and parameters of the inner binary population. | 224 | [
"10.1093/mnras/stad3393"
] | 20,240,601 | [
"2024MNRAS.527.4573B"
] | In another study, [REF] found Newtonian gravity to be strongly preferred ( 16 ) over MOND, with relatively weak sensitivity to the assumed eccentricity distribution and parameters of the inner binary population. |
10.1016/j.newar.2024.101694 | Belokurov et al. (2020) showed that selecting targets with large ruwe (e.g. ruwe > 1 . 4 ) yields a sample of sources preferentially in regions of the color-magnitude diagram where binaries are expected to be concentrated ( Fig. 5 , right panel). | showed that selecting targets with large ruwe (e.g. ruwe > 1 . 4 ) yields a sample of sources preferentially in regions of the color-magnitude diagram where binaries are expected to be concentrated ( Fig. 5 , right panel). | 250 | [
"10.1093/mnras/staa1522"
] | 20,240,601 | [
"2020MNRAS.496.1922B"
] | [REF] showed that selecting targets with large ruwe (e.g. ruwe > 1 . 4 ) yields a sample of sources preferentially in regions of the color-magnitude diagram where binaries are expected to be concentrated ( Fig. 5 , right panel). |
10.1016/j.newar.2024.101694 | For binaries with orbital periods shorter than the Gaia observational baseline, the expected amplitude of the ruwe signal due to an unresolved binary scales approximately linearly with the angular size of the photocenter orbit (e.g. Stassun and Torres, 2021 ). | For binaries with orbital periods shorter than the Gaia observational baseline, the expected amplitude of the ruwe signal due to an unresolved binary scales approximately linearly with the angular size of the photocenter orbit (e.g. ). | 253 | [
"10.3847/2041-8213/abdaad"
] | 20,240,601 | [
"2021ApJ...907L..33S"
] | For binaries with orbital periods shorter than the Gaia observational baseline, the expected amplitude of the ruwe signal due to an unresolved binary scales approximately linearly with the angular size of the photocenter orbit (e.g. [REF] ). |
10.1016/j.newar.2024.101694 | Korol et al. (2022) studied the ruwe distributions of nearby white dwarfs and found evidence for a dearth of WD+WD binaries with au-scale orbits (i.e., the separation range to which ruwe is most sensitive), presumably because most orbits in this separation range are cleared out by common envelope evolution. | studied the ruwe distributions of nearby white dwarfs and found evidence for a dearth of WD+WD binaries with au-scale orbits (i.e., the separation range to which ruwe is most sensitive), presumably because most orbits in this separation range are cleared out by common envelope evolution. | 256 | [
"10.1093/mnras/stac1686"
] | 20,240,601 | [
"2022MNRAS.515.1228K"
] | [REF] studied the ruwe distributions of nearby white dwarfs and found evidence for a dearth of WD+WD binaries with au-scale orbits (i.e., the separation range to which ruwe is most sensitive), presumably because most orbits in this separation range are cleared out by common envelope evolution. |
10.1016/j.newar.2024.101694 | The gravitational effects of the directly-imaged planet Pic b on its host star, for example, were detected by Kervella et al. (2019) with high significance. | The gravitational effects of the directly-imaged planet Pic b on its host star, for example, were detected by with high significance. | 276 | [
"10.1051/0004-6361/201834371"
] | 20,240,601 | [
"2019A&A...623A..72K"
] | The gravitational effects of the directly-imaged planet Pic b on its host star, for example, were detected by [REF] with high significance. |
10.1016/j.newar.2024.101694 | The right panel of Fig. 7 shows how q depends on the mass ratio for typical main-sequence stars: using a 300-Myr old MIST isochrone with solar metallicity ( Choi et al., 2016 ), I plot the predicted a 0 for a Sun-like star with a range of main-sequence companions. | The right panel of Fig. 7 shows how q depends on the mass ratio for typical main-sequence stars: using a 300-Myr old MIST isochrone with solar metallicity ( ), I plot the predicted a 0 for a Sun-like star with a range of main-sequence companions. | 323 | [
"10.3847/0004-637X/823/2/102"
] | 20,240,601 | [
"2016ApJ...823..102C"
] | The right panel of Fig. 7 shows how q depends on the mass ratio for typical main-sequence stars: using a 300-Myr old MIST isochrone with solar metallicity ( [REF] ), I plot the predicted a 0 for a Sun-like star with a range of main-sequence companions. |
10.1016/j.newar.2024.101694 | Acceleration solutions may eventually become powerful for identifying stellar- or even intermediate-mass black holes from partial orbits ( Andrews et al., 2023 ). | Acceleration solutions may eventually become powerful for identifying stellar- or even intermediate-mass black holes from partial orbits ( ). | 348 | [
"10.3847/1538-4357/acbb5f"
] | 20,240,601 | [
"2023ApJ...946..111A"
] | Acceleration solutions may eventually become powerful for identifying stellar- or even intermediate-mass black holes from partial orbits ( [REF] ). |
10.1016/j.newar.2024.101694 | Breivik et al. (2017) made the first attempt to incorporate binary evolution via population synthesis simulations in predictions for the Gaia BH population. | made the first attempt to incorporate binary evolution via population synthesis simulations in predictions for the Gaia BH population. | 358 | [
"10.3847/2041-8213/aa97d5"
] | 20,240,601 | [
"2017ApJ...850L..13B"
] | [REF] made the first attempt to incorporate binary evolution via population synthesis simulations in predictions for the Gaia BH population. |
10.1016/j.newar.2024.101694 | 5.1.3 Planets and brown dwarfs Gaia has been predicted to eventually discover between 1 0 4 and 1 0 5 exoplanets via astrometric wobble of their host stars ( Perryman et al., 2014 ). | 5.1.3 Planets and brown dwarfs Gaia has been predicted to eventually discover between 1 0 4 and 1 0 5 exoplanets via astrometric wobble of their host stars ( ). | 424 | [
"10.1088/0004-637X/797/1/14"
] | 20,240,601 | [
"2014ApJ...797...14P"
] | 5.1.3 Planets and brown dwarfs Gaia has been predicted to eventually discover between 1 0 4 and 1 0 5 exoplanets via astrometric wobble of their host stars ( [REF] ). |
10.1016/j.newar.2024.101694 | Winterhalder et al. (2024) showed that the widest astrometric binaries, with separations 30 mas , can be resolved with GRAVITY interferometry. | showed that the widest astrometric binaries, with separations 30 mas , can be resolved with GRAVITY interferometry. | 433 | [
"10.1051/0004-6361/202450018"
] | 20,240,601 | [
"2024A&A...688A..44W"
] | [REF] showed that the widest astrometric binaries, with separations 30 mas , can be resolved with GRAVITY interferometry. |
10.1016/j.newar.2024.101694 | Bashi et al. (2022) showed that the rate of spurious orbital solutions among the spectroscopic orbital solutions is generally highest at short periods; they designed a quality metric to filter out spurious solutions that combines information contained in several different Gaia quality flags. | showed that the rate of spurious orbital solutions among the spectroscopic orbital solutions is generally highest at short periods; they designed a quality metric to filter out spurious solutions that combines information contained in several different Gaia quality flags. | 443 | [
"10.1093/mnras/stac2928"
] | 20,240,601 | [
"2022MNRAS.517.3888B"
] | [REF] showed that the rate of spurious orbital solutions among the spectroscopic orbital solutions is generally highest at short periods; they designed a quality metric to filter out spurious solutions that combines information contained in several different Gaia quality flags. |
10.1016/j.newar.2024.101694 | Gomel et al. (2023) used this fact to select a sample of 6000 candidate ellipsoidal variables that may host a compact object companion, including 262 high-confidence systems with minimum mass ratios significantly larger than one. | used this fact to select a sample of 6000 candidate ellipsoidal variables that may host a compact object companion, including 262 high-confidence systems with minimum mass ratios significantly larger than one. | 472 | [
"10.1051/0004-6361/202243782"
] | 20,240,601 | [
"2023A&A...674A..34G"
] | [REF] used this fact to select a sample of 6000 candidate ellipsoidal variables that may host a compact object companion, including 262 high-confidence systems with minimum mass ratios significantly larger than one. |
10.1016/j.newar.2024.101694 | Nagarajan et al. (2023) investigated the nature of this sample in more detail, carrying out spectroscopic follow-up on a sub-sample of the candidates. | investigated the nature of this sample in more detail, carrying out spectroscopic follow-up on a sub-sample of the candidates. | 473 | [
"10.1093/mnras/stad2130"
] | 20,240,601 | [
"2023MNRAS.524.4367N"
] | [REF] investigated the nature of this sample in more detail, carrying out spectroscopic follow-up on a sub-sample of the candidates. |
10.1016/j.newar.2024.101694 | Pala et al. (2020) assembled a nearly-complete sample of 42 cataclysmic variables within 150 pc (bottom panel of Fig. 12 ), from which they measured a CV space density of = 4 . | assembled a nearly-complete sample of 42 cataclysmic variables within 150 pc (bottom panel of Fig. 12 ), from which they measured a CV space density of = 4 . | 482 | [
"10.1093/mnras/staa764"
] | 20,240,601 | [
"2020MNRAS.494.3799P"
] | [REF] assembled a nearly-complete sample of 42 cataclysmic variables within 150 pc (bottom panel of Fig. 12 ), from which they measured a CV space density of = 4 . |
10.1016/j.newar.2024.101694 | Pala et al. (2020) found that magnetic CVs (polars and intermediate polars) make up 36% of the 150 pc sample a much larger fraction than in earlier CV samples that were not volume limited. | found that magnetic CVs (polars and intermediate polars) make up 36% of the 150 pc sample a much larger fraction than in earlier CV samples that were not volume limited. | 485 | [
"10.1093/mnras/staa764"
] | 20,240,601 | [
"2020MNRAS.494.3799P"
] | [REF] found that magnetic CVs (polars and intermediate polars) make up 36% of the 150 pc sample a much larger fraction than in earlier CV samples that were not volume limited. |
10.1016/j.newar.2024.101694 | Linking them to triples (if they have tertiary companions, as e.g. Tokovinin et al. 2006 find most close binaries do) implies that original inner periods in those triples were of a few days. | Linking them to triples (if they have tertiary companions, as e.g. find most close binaries do) implies that original inner periods in those triples were of a few days. | 500 | [
"10.1051/0004-6361:20054427"
] | 20,240,601 | [
"2006A&A...450..681T"
] | Linking them to triples (if they have tertiary companions, as e.g. [REF] find most close binaries do) implies that original inner periods in those triples were of a few days. |
10.1016/j.newar.2024.101694 | 6.4 Hypervelocity white dwarfs By using Gaia astrometry to search for stars with high proper motions and large distances, Shen et al. (2018) identified a population of hypervelocity stars launched from thermonuclear supernovae in close WD binaries. | 6.4 Hypervelocity white dwarfs By using Gaia astrometry to search for stars with high proper motions and large distances, identified a population of hypervelocity stars launched from thermonuclear supernovae in close WD binaries. | 501 | [
"10.3847/1538-4357/aad55b"
] | 20,240,601 | [
"2018ApJ...865...15S"
] | 6.4 Hypervelocity white dwarfs By using Gaia astrometry to search for stars with high proper motions and large distances, [REF] identified a population of hypervelocity stars launched from thermonuclear supernovae in close WD binaries. |
10.1016/j.newar.2024.101694 | The flight path of the youngest such star identified by Shen et al. (2018) can be traced back to a type Ia supernova remnant ( Fig. 13 , left panel), in strong support of this formation model. | The flight path of the youngest such star identified by can be traced back to a type Ia supernova remnant ( Fig. 13 , left panel), in strong support of this formation model. | 503 | [
"10.3847/1538-4357/aad55b"
] | 20,240,601 | [
"2018ApJ...865...15S"
] | The flight path of the youngest such star identified by [REF] can be traced back to a type Ia supernova remnant ( Fig. 13 , left panel), in strong support of this formation model. |
10.1016/j.newar.2024.101694 | Raddi et al. (2019) propose that the slower of these objects (LP 40-365 stars) are partially burned runaway accretors from single-degenerate thermonuclear supernovae, while the higher-velocity objects are runaway donors from double-degenerate binaries. | propose that the slower of these objects (LP 40-365 stars) are partially burned runaway accretors from single-degenerate thermonuclear supernovae, while the higher-velocity objects are runaway donors from double-degenerate binaries. | 505 | [
"10.1093/mnras/stz1618"
] | 20,240,601 | [
"2019MNRAS.489.1489R"
] | [REF] propose that the slower of these objects (LP 40-365 stars) are partially burned runaway accretors from single-degenerate thermonuclear supernovae, while the higher-velocity objects are runaway donors from double-degenerate binaries. |
10.1016/j.newar.2024.101694 | These data will foreseeable yield good constraints on the orbits of binaries with periods reaching up to 20 years, and useful acceleration constraints at even longer periods (e.g. Andrews et al., 2023 ). | These data will foreseeable yield good constraints on the orbits of binaries with periods reaching up to 20 years, and useful acceleration constraints at even longer periods (e.g. ). | 523 | [
"10.3847/1538-4357/acbb5f"
] | 20,240,601 | [
"2023ApJ...946..111A"
] | These data will foreseeable yield good constraints on the orbits of binaries with periods reaching up to 20 years, and useful acceleration constraints at even longer periods (e.g. [REF] ). |
10.1146/annurev.astro.46.060407.145222 | We note that Lodders (2003) adopted a somewhat larger correction, 0.074 dex, than that of Turcotte Wimmer-Schweingruber (2002) . | We note that adopted a somewhat larger correction, 0.074 dex, than that of . | 484 | [
"10.1086/375492",
"10.1029/2002JA009418"
] | 20,090,901 | [
"2003ApJ...591.1220L",
"2002JGRA..107.1442T"
] | We note that [REF] adopted a somewhat larger correction, 0.074 dex, than that of [REF] . |
10.1146/annurev.astro.46.060407.145222 | In other words, the solar metallicity is no longer the canonical 2% recommended by Anders Grevesse (1989) but rather a substantially smaller 1.4%. | In other words, the solar metallicity is no longer the canonical 2% recommended by but rather a substantially smaller 1.4%. | 489 | [
"10.1016/0016-7037(89)90286-X"
] | 20,090,901 | [
"1989GeCoA..53..197A"
] | In other words, the solar metallicity is no longer the canonical 2% recommended by [REF] but rather a substantially smaller 1.4%. |
10.1146/annurev.astro.46.060407.145222 | Our metallicity reverses this declining trend of Z with time by being slightly larger than advocated by Asplund, Grevesse Sauval (2005) , which is mainly the result of the somewhat higher C, N, O, Ne, and Fe abundances. | Our metallicity reverses this declining trend of Z with time by being slightly larger than advocated by , which is mainly the result of the somewhat higher C, N, O, Ne, and Fe abundances. | 492 | [
"10.1051/0004-6361:20041951"
] | 20,090,901 | [
"2005A&A...431..693A"
] | Our metallicity reverses this declining trend of Z with time by being slightly larger than advocated by [REF] , which is mainly the result of the somewhat higher C, N, O, Ne, and Fe abundances. |
10.1146/annurev.astro.46.060407.145222 | Finally, from Table 4 it is clear that the surface He abundance employed by Lodders (2003) is too low on account of adopting a too efficient elemental diffusion. | Finally, from Table 4 it is clear that the surface He abundance employed by is too low on account of adopting a too efficient elemental diffusion. | 495 | [
"10.1086/375492"
] | 20,090,901 | [
"2003ApJ...591.1220L"
] | Finally, from Table 4 it is clear that the surface He abundance employed by [REF] is too low on account of adopting a too efficient elemental diffusion. |
10.1146/annurev.astro.46.060407.145222 | The most primitive, undifferentiated meteorites in this respect are the so-called C I (or C1) carbonaceous chondrites, of which only five are known: the Alais, Ivuna (after which this class of meteorites is named), Orgueil, Revelstoke, and Tonk meteorites ( Lodders 2003 ). | The most primitive, undifferentiated meteorites in this respect are the so-called C I (or C1) carbonaceous chondrites, of which only five are known: the Alais, Ivuna (after which this class of meteorites is named), Orgueil, Revelstoke, and Tonk meteorites ( ). | 499 | [
"10.1086/375492"
] | 20,090,901 | [
"2003ApJ...591.1220L"
] | The most primitive, undifferentiated meteorites in this respect are the so-called C I (or C1) carbonaceous chondrites, of which only five are known: the Alais, Ivuna (after which this class of meteorites is named), Orgueil, Revelstoke, and Tonk meteorites ( [REF] ). |
10.1146/annurev.astro.46.060407.145222 | We note a significant improvement for W compared to previous compilations of the solar chemical composition [Δlog ε = +0.49 dex in Asplund, Grevesse Sauval (2005) , whereas here the difference amounts to +0.20 dex]; we suspect that unidentified blends and/or erroneous continuum placement may be at fault for the persist... | We note a significant improvement for W compared to previous compilations of the solar chemical composition [Δlog ε = +0.49 dex in , whereas here the difference amounts to +0.20 dex]; we suspect that unidentified blends and/or erroneous continuum placement may be at fault for the persisting discrepancy, likewise for R... | 521 | [
"10.1051/0004-6361:20041951"
] | 20,090,901 | [
"2005A&A...431..693A"
] | We note a significant improvement for W compared to previous compilations of the solar chemical composition [Δlog ε = +0.49 dex in [REF] , whereas here the difference amounts to +0.20 dex]; we suspect that unidentified blends and/or erroneous continuum placement may be at fault for the persisting discrepancy, likewise ... |
10.1146/annurev.astro.46.060407.145222 | The remaining three elements, Rh, Ag, and Pb, have had their photospheric values determined from transitions originating either in the ground state or from low-excitation levels of the neutral species (also true for Pd, W, and Au), which are prone to non-LTE effects in their excitation and ionization populations ( Aspl... | The remaining three elements, Rh, Ag, and Pb, have had their photospheric values determined from transitions originating either in the ground state or from low-excitation levels of the neutral species (also true for Pd, W, and Au), which are prone to non-LTE effects in their excitation and ionization populations ( ). | 523 | [
"10.1051/0004-6361:20041951"
] | 20,090,901 | [
"2005A&A...431..693A"
] | The remaining three elements, Rh, Ag, and Pb, have had their photospheric values determined from transitions originating either in the ground state or from low-excitation levels of the neutral species (also true for Pd, W, and Au), which are prone to non-LTE effects in their excitation and ionization populations ( [REF... |
10.1146/annurev.astro.46.060407.145222 | It is unclear whether the solution can be found in the solar or B star analyses or, if a real difference indeed exists, perhaps due to infall of low-metallicity gas to the Solar Neighborhood or due to Galactic orbital migration ( Schönrich Binney 2009 ). | It is unclear whether the solution can be found in the solar or B star analyses or, if a real difference indeed exists, perhaps due to infall of low-metallicity gas to the Solar Neighborhood or due to Galactic orbital migration ( ). | 541 | [
"10.1111/j.1365-2966.2009.14750.x"
] | 20,090,901 | [
"2009MNRAS.396..203S"
] | It is unclear whether the solution can be found in the solar or B star analyses or, if a real difference indeed exists, perhaps due to infall of low-metallicity gas to the Solar Neighborhood or due to Galactic orbital migration ( [REF] ). |
10.1146/annurev.astro.46.060407.145222 | In Table 5 we provide the values from Esteban et al. (2004 , 2005) and García-Rojas Esteban (2007) interpolated to a Galacto-centric radius of 8 kpc. | In Table 5 we provide the values from and interpolated to a Galacto-centric radius of 8 kpc. | 550 | [
"10.1111/j.1365-2966.2004.08313.x",
"10.1086/426889",
"10.1086/521871"
] | 20,090,901 | [
"2004MNRAS.355..229E",
"2005ApJ...618L..95E",
"2007ApJ...670..457G"
] | In Table 5 we provide the values from [REF] and [REF] interpolated to a Galacto-centric radius of 8 kpc. |
10.1146/annurev.astro.46.060407.145222 | For C and O this somewhat uncertain dust correction amounts to ≈0.1 dex in Orion ( Esteban et al. 2004 ). | For C and O this somewhat uncertain dust correction amounts to ≈0.1 dex in Orion ( ). | 555 | [
"10.1111/j.1365-2966.2004.08313.x"
] | 20,090,901 | [
"2004MNRAS.355..229E"
] | For C and O this somewhat uncertain dust correction amounts to ≈0.1 dex in Orion ( [REF] ). |
10.1146/annurev.astro.46.060407.145222 | Because of the generally lower temperatures encountered and the consequentially larger degree of dust condensation, the interstellar medium is a less reliable chemical composition gauge than H ii regions ( Jenkins 2004 ). | Because of the generally lower temperatures encountered and the consequentially larger degree of dust condensation, the interstellar medium is a less reliable chemical composition gauge than H ii regions ( ). | 558 | [
"10.48550/arXiv.astro-ph/0309651"
] | 20,090,901 | [
"2004oee..symp..336J"
] | Because of the generally lower temperatures encountered and the consequentially larger degree of dust condensation, the interstellar medium is a less reliable chemical composition gauge than H ii regions ( [REF] ). |
10.1146/annurev.astro.46.060407.145222 | Indeed, rather than setting constraints on the solar abundances, the Sun is often used to infer the amount in the solid phase in the interstellar medium (e.g., Sofia Meyer 2001 ). | Indeed, rather than setting constraints on the solar abundances, the Sun is often used to infer the amount in the solid phase in the interstellar medium (e.g., ). | 559 | [
"10.1086/321715"
] | 20,090,901 | [
"2001ApJ...554L.221S"
] | Indeed, rather than setting constraints on the solar abundances, the Sun is often used to infer the amount in the solid phase in the interstellar medium (e.g., [REF] ). |
10.1146/annurev.astro.46.060407.145222 | Also listed in Table 5 are predictions from models of Galactic chemical evolution ( Chiappini, Romano Matteucci 2003 ). | Also listed in Table 5 are predictions from models of Galactic chemical evolution ( ). | 563 | [
"10.1046/j.1365-8711.2003.06154.x"
] | 20,090,901 | [
"2003MNRAS.339...63C"
] | Also listed in Table 5 are predictions from models of Galactic chemical evolution ( [REF] ). |
10.1146/annurev.astro.46.060407.145222 | An alternative explanation would be recent Galactic infall of more pristine gas or Galactic orbital migration ( Schönrich Binney 2009 ). | An alternative explanation would be recent Galactic infall of more pristine gas or Galactic orbital migration ( ). | 570 | [
"10.1111/j.1365-2966.2009.14750.x"
] | 20,090,901 | [
"2009MNRAS.396..203S"
] | An alternative explanation would be recent Galactic infall of more pristine gas or Galactic orbital migration ( [REF] ). |
10.1146/annurev.astro.46.060407.145222 | The inferred depth of the convection zone is now too shallow: R BCZ ≈ 0.725 R ⊙ instead of the helioseismic measurement 0.7133 ± 0.0005 R ⊙ ( Basu Antia 2004 ). | The inferred depth of the convection zone is now too shallow: R BCZ ≈ 0.725 R ⊙ instead of the helioseismic measurement 0.7133 ± 0.0005 R ⊙ ( ). | 585 | [
"10.1086/421110"
] | 20,090,901 | [
"2004ApJ...606L..85B"
] | The inferred depth of the convection zone is now too shallow: R BCZ ≈ 0.725 R ⊙ instead of the helioseismic measurement 0.7133 ± 0.0005 R ⊙ ( [REF] ). |
10.1146/annurev.astro.46.060407.145222 | Furthermore, the resulting He abundance when calibrating solar interior models to achieve the correct solar luminosity and temperature at the solar age is similarly inconsistent with the value inferred from helioseismology (see Section 3.9): Y S ≈ 0.238 compared to the observed 0.2485 ± 0.0034 ( Basu Antia 2004 ), wher... | Furthermore, the resulting He abundance when calibrating solar interior models to achieve the correct solar luminosity and temperature at the solar age is similarly inconsistent with the value inferred from helioseismology (see Section 3.9): Y S ≈ 0.238 compared to the observed 0.2485 ± 0.0034 ( ), where Y S is the pr... | 586 | [
"10.1086/421110"
] | 20,090,901 | [
"2004ApJ...606L..85B"
] | Furthermore, the resulting He abundance when calibrating solar interior models to achieve the correct solar luminosity and temperature at the solar age is similarly inconsistent with the value inferred from helioseismology (see Section 3.9): Y S ≈ 0.238 compared to the observed 0.2485 ± 0.0034 ( [REF] ), where Y S is t... |
10.1146/annurev.astro.46.060407.145222 | Furthermore, though this may remedy the sound speed discrepancy, problems still remain in terms of the He abundance and depth of the convection zone ( Montalbán et al. 2004 ; Guzik, Watson Cox 2005 ; Yang Bi 2007 ). | Furthermore, though this may remedy the sound speed discrepancy, problems still remain in terms of the He abundance and depth of the convection zone ( ). | 599 | [
"10.48550/arXiv.astro-ph/0408055",
"10.1086/430438",
"10.1086/513694"
] | 20,090,901 | [
"2004ESASP.559..574M",
"2005ApJ...627.1049G",
"2007ApJ...658L..67Y"
] | Furthermore, though this may remedy the sound speed discrepancy, problems still remain in terms of the He abundance and depth of the convection zone ( [REF] ). |
10.1146/annurev.astro.46.060407.145222 | A hypothetical late accretion of metal-depleted gas during the formation of the Sun runs into the same trouble ( Guzik, Watson Cox 2005 , Castro, Vauclair Richard 2007 ). | A hypothetical late accretion of metal-depleted gas during the formation of the Sun runs into the same trouble ( ). | 600 | [
"10.1086/430438",
"10.1051/0004-6361:20066327"
] | 20,090,901 | [
"2005ApJ...627.1049G",
"2007A&A...463..755C"
] | A hypothetical late accretion of metal-depleted gas during the formation of the Sun runs into the same trouble ( [REF] ). |
10.1146/annurev.astro.46.060407.145222 | There was initial excitement when Drake Testa (2005) argued for exactly such an increase in Ne on the basis of inferences from coronal spectroscopy of other stars, but there is in fact little support for this idea, as explained in Section 3.9. | There was initial excitement when argued for exactly such an increase in Ne on the basis of inferences from coronal spectroscopy of other stars, but there is in fact little support for this idea, as explained in Section 3.9. | 603 | [
"10.1038/nature03803"
] | 20,090,901 | [
"2005Natur.436..525D"
] | There was initial excitement when [REF] argued for exactly such an increase in Ne on the basis of inferences from coronal spectroscopy of other stars, but there is in fact little support for this idea, as explained in Section 3.9. |
10.1146/annurev.astro.46.060407.145222 | The here recommended abundance of Ne is slightly higher than in Asplund, Grevesse Sauval (2005) , as are our recommended values for C, N, and O. This shift only partly allays the solar modeling discrepancy, as seen in Figure 8 . | The here recommended abundance of Ne is slightly higher than in , as are our recommended values for C, N, and O. This shift only partly allays the solar modeling discrepancy, as seen in Figure 8 . | 604 | [
"10.1051/0004-6361:20041951"
] | 20,090,901 | [
"2005A&A...431..693A"
] | The here recommended abundance of Ne is slightly higher than in [REF] , as are our recommended values for C, N, and O. This shift only partly allays the solar modeling discrepancy, as seen in Figure 8 . |
10.1146/annurev.astro.46.060407.145222 | Although the neutrino fluxes cannot be directly associated with abundances of individual elements, the relevant neutrino channels depend most sensitively on C, N, O, Si, and Fe ( Bahcall Serenelli 2005 ). | Although the neutrino fluxes cannot be directly associated with abundances of individual elements, the relevant neutrino channels depend most sensitively on C, N, O, Si, and Fe ( ). | 620 | [
"10.1086/426070"
] | 20,090,901 | [
"2005ApJ...618.1049B"
] | Although the neutrino fluxes cannot be directly associated with abundances of individual elements, the relevant neutrino channels depend most sensitively on C, N, O, Si, and Fe ( [REF] ). |
10.1146/annurev.astro.46.060407.145222 | The values we recommend for the most abundant metals C, N, O, Ne, and Fe are significantly smaller (by ∼0.2 dex) than those advocated in the widely used compilation of Anders Grevesse (1989) . | The values we recommend for the most abundant metals C, N, O, Ne, and Fe are significantly smaller (by ∼0.2 dex) than those advocated in the widely used compilation of . | 629 | [
"10.1016/0016-7037(89)90286-X"
] | 20,090,901 | [
"1989GeCoA..53..197A"
] | The values we recommend for the most abundant metals C, N, O, Ne, and Fe are significantly smaller (by ∼0.2 dex) than those advocated in the widely used compilation of [REF] . |
10.1146/annurev.astro.46.060407.145222 | The discordance has been alleviated somewhat relative to the recommended values in Asplund, Grevesse Sauval (2005) , but it nevertheless remains a significant discrepancy in urgent need of resolution. | The discordance has been alleviated somewhat relative to the recommended values in , but it nevertheless remains a significant discrepancy in urgent need of resolution. | 642 | [
"10.1051/0004-6361:20041951"
] | 20,090,901 | [
"2005A&A...431..693A"
] | The discordance has been alleviated somewhat relative to the recommended values in [REF] , but it nevertheless remains a significant discrepancy in urgent need of resolution. |
10.1146/annurev.astro.46.060407.145222 | As discussed by Asplund (2005) , even though departures from LTE are expected to be relatively serene in the Sun, one should always expect non-LTE abundance corrections at around the 0.05 dex level; indeed in many cases the effects will be significantly more severe. | As discussed by , even though departures from LTE are expected to be relatively serene in the Sun, one should always expect non-LTE abundance corrections at around the 0.05 dex level; indeed in many cases the effects will be significantly more severe. | 659 | [
"10.1051/0004-6361:20041951"
] | 20,090,901 | [
"2005A&A...431..693A"
] | As discussed by [REF] , even though departures from LTE are expected to be relatively serene in the Sun, one should always expect non-LTE abundance corrections at around the 0.05 dex level; indeed in many cases the effects will be significantly more severe. |
10.1146/annurev-astro-081811-125521 | The Bondi accretion radius is resolved in Chandra X-ray images of some of the nearest objects, such as M87 ( Di Matteo et al. 2003 ), enabling the temperature and density profiles to be estimated and, thus, the accretion rate to be determined. | The Bondi accretion radius is resolved in Chandra X-ray images of some of the nearest objects, such as M87 ( ), enabling the temperature and density profiles to be estimated and, thus, the accretion rate to be determined. | 483 | [
"10.1086/344504"
] | 20,120,901 | [
"2003ApJ...582..133D"
] | The Bondi accretion radius is resolved in Chandra X-ray images of some of the nearest objects, such as M87 ( [REF] ), enabling the temperature and density profiles to be estimated and, thus, the accretion rate to be determined. |
10.1146/annurev-astro-081811-125521 | Allen et al. (2006) have studied a sample in which the kinetic power can be estimated from bubbles and compare this with the Bondi accretion rate. | have studied a sample in which the kinetic power can be estimated from bubbles and compare this with the Bondi accretion rate. | 485 | [
"10.1111/j.1365-2966.2006.10778.x"
] | 20,120,901 | [
"2006MNRAS.372...21A"
] | [REF] have studied a sample in which the kinetic power can be estimated from bubbles and compare this with the Bondi accretion rate. |
10.1146/annurev-astro-081811-125521 | 4. BARYON PROFILES AT DIFFERENT MASS SCALES AND ACTIVE GALACTIC NUCLEI FEEDBACK Early predictions for the relationship between the X-ray luminosity and temperature of intracluster gas indicated L ∝ T 2 , based on gas falling into dark matter potential wells of different total masses ( Kaiser 1986 ). | 4. BARYON PROFILES AT DIFFERENT MASS SCALES AND ACTIVE GALACTIC NUCLEI FEEDBACK Early predictions for the relationship between the X-ray luminosity and temperature of intracluster gas indicated L ∝ T 2 , based on gas falling into dark matter potential wells of different total masses ( ). | 496 | [
"10.1093/mnras/222.2.323"
] | 20,120,901 | [
"1986MNRAS.222..323K"
] | 4. BARYON PROFILES AT DIFFERENT MASS SCALES AND ACTIVE GALACTIC NUCLEI FEEDBACK Early predictions for the relationship between the X-ray luminosity and temperature of intracluster gas indicated L ∝ T 2 , based on gas falling into dark matter potential wells of different total masses ( [REF] ). |
10.1146/annurev-astro-081811-125521 | Observations show otherwise with a relation closer to L ∝ T 2.7 for clusters with temperatures in the range of 3.5–10 keV ( Markevitch 1998 ). | Observations show otherwise with a relation closer to L ∝ T 2.7 for clusters with temperatures in the range of 3.5–10 keV ( ). | 498 | [
"10.1086/306080"
] | 20,120,901 | [
"1998ApJ...504...27M"
] | Observations show otherwise with a relation closer to L ∝ T 2.7 for clusters with temperatures in the range of 3.5–10 keV ( [REF] ). |
10.1146/annurev-astro-081811-125521 | The gas fraction (baryon mass versus total mass) rises outward in clusters and approaches the cosmic value toward the virial radius (e.g., Allen et al. 2008 ; Vikhlinin et al. 2006 ). | The gas fraction (baryon mass versus total mass) rises outward in clusters and approaches the cosmic value toward the virial radius ( ). | 504 | [
"10.1111/j.1365-2966.2007.12610.x",
"10.1086/500288"
] | 20,120,901 | [
"2008MNRAS.383..879A",
"2006ApJ...640..691V"
] | The gas fraction (baryon mass versus total mass) rises outward in clusters and approaches the cosmic value toward the virial radius ([REF] ). |
10.1146/annurev-astro-081811-125521 | Gonzalez, Zaritsky Zabludoff (2007) find an increasing stellar fraction with decreasing group/cluster mass, peaking below 10 14 M ⊙ , where stellar and gas masses are equal. | find an increasing stellar fraction with decreasing group/cluster mass, peaking below 10 14 M ⊙ , where stellar and gas masses are equal. | 506 | [
"10.1086/519729"
] | 20,120,901 | [
"2007ApJ...666..147G"
] | [REF] find an increasing stellar fraction with decreasing group/cluster mass, peaking below 10 14 M ⊙ , where stellar and gas masses are equal. |
10.1146/annurev-astro-081811-125521 | They also approach the cosmic value at the virial radius ( Humphrey et al. 2012 ). | They also approach the cosmic value at the virial radius ( ). | 508 | [
"10.1088/0004-637X/748/1/11"
] | 20,120,901 | [
"2012ApJ...748...11H"
] | They also approach the cosmic value at the virial radius ( [REF] ). |
10.1146/annurev-astro-081811-125521 | If the injection was after the group or cluster was formed, then about 1–3 keV per nucleon is required ( Wu, Fabian Nulsen 2000 ; Lapi, Cavaliere Menci 2005 ), which clearly will have a major impact on low-temperature clusters and groups. | If the injection was after the group or cluster was formed, then about 1–3 keV per nucleon is required ( ), which clearly will have a major impact on low-temperature clusters and groups. | 511 | [
"10.1046/j.1365-8711.2000.03828.x",
"10.1086/426376"
] | 20,120,901 | [
"2000MNRAS.318..889W",
"2005ApJ...619...60L"
] | If the injection was after the group or cluster was formed, then about 1–3 keV per nucleon is required ( [REF] ), which clearly will have a major impact on low-temperature clusters and groups. |
10.1146/annurev-astro-081811-125521 | Young et al. (2011) find from this approach that continual feedback is preferable to preheating. | find from this approach that continual feedback is preferable to preheating. | 514 | [
"10.1111/j.1365-2966.2010.18165.x"
] | 20,120,901 | [
"2011MNRAS.413..691Y"
] | [REF] find from this approach that continual feedback is preferable to preheating. |
10.1146/annurev-astro-081811-125521 | These Fanaroff-Riley Class II objects have lobes that extend many hundreds of kiloparsecs from the active nucleus and, due to extensive losses (synchrotron cooling, adiabatic expansion, and inverse Compton scattering on the cosmic microwave background), are only readily observed in the radio band when they are young ( ... | These Fanaroff-Riley Class II objects have lobes that extend many hundreds of kiloparsecs from the active nucleus and, due to extensive losses (synchrotron cooling, adiabatic expansion, and inverse Compton scattering on the cosmic microwave background), are only readily observed in the radio band when they are young ( ... | 517 | [
"10.1038/20612"
] | 20,120,901 | [
"1999Natur.399..330B"
] | These Fanaroff-Riley Class II objects have lobes that extend many hundreds of kiloparsecs from the active nucleus and, due to extensive losses (synchrotron cooling, adiabatic expansion, and inverse Compton scattering on the cosmic microwave background), are only readily observed in the radio band when they are young ( ... |
10.1146/annurev-astro-081811-125521 | The lobe energies estimated from radio and X-ray ( Erlund et al. 2006 ) observations are high, ranging from 10 60 –10 62+ erg with a large uncertainty in the energy stored in protons, which should increase the total energy. | The lobe energies estimated from radio and X-ray ( ) observations are high, ranging from 10 60 –10 62+ erg with a large uncertainty in the energy stored in protons, which should increase the total energy. | 518 | [
"10.1111/j.1365-2966.2006.10660.x"
] | 20,120,901 | [
"2006MNRAS.371...29E"
] | The lobe energies estimated from radio and X-ray ( [REF] ) observations are high, ranging from 10 60 –10 62+ erg with a large uncertainty in the energy stored in protons, which should increase the total energy. |
10.1146/annurev-astro-081811-125521 | The galaxy dies and any later infalling or cooling gas is heated by jetted, maintenance-mode feedback (e.g., Churazov et al. 2005 ). | The galaxy dies and any later infalling or cooling gas is heated by jetted, maintenance-mode feedback (e.g., ). | 528 | [
"10.1111/j.1745-3933.2005.00093.x"
] | 20,120,901 | [
"2005MNRAS.363L..91C"
] | The galaxy dies and any later infalling or cooling gas is heated by jetted, maintenance-mode feedback (e.g., [REF] ). |
10.1146/annurev-astro-081811-125521 | Although they are not important sources of feedback in a galaxy, some BHBs do blow bubbles (e.g., Gallo et al. 2005 ). | Although they are not important sources of feedback in a galaxy, some BHBs do blow bubbles (e.g., ). | 532 | [
"10.1038/nature03879"
] | 20,120,901 | [
"2005Natur.436..819G"
] | Although they are not important sources of feedback in a galaxy, some BHBs do blow bubbles (e.g., [REF] ). |
10.1146/annurev-astro-081811-125521 | The radio emission scales in a more complex manner along a fundamental plane ( Merloni, Heinz Di Matteo 2003 ), but the general pattern may remain for AGN. | The radio emission scales in a more complex manner along a fundamental plane ( ), but the general pattern may remain for AGN. | 537 | [
"10.1046/j.1365-2966.2003.07017.x"
] | 20,120,901 | [
"2003MNRAS.345.1057M"
] | The radio emission scales in a more complex manner along a fundamental plane ( [REF] ), but the general pattern may remain for AGN. |
10.1146/annurev-astro-081811-125521 | An attractive possibility is that the radiative mode shaped the overall galaxy and black hole mass at early times, and the kinetic mode has since maintained that situation where needed ( Churazov et al. 2005 ). | An attractive possibility is that the radiative mode shaped the overall galaxy and black hole mass at early times, and the kinetic mode has since maintained that situation where needed ( ). | 582 | [
"10.1111/j.1745-3933.2005.00093.x"
] | 20,120,901 | [
"2005MNRAS.363L..91C"
] | An attractive possibility is that the radiative mode shaped the overall galaxy and black hole mass at early times, and the kinetic mode has since maintained that situation where needed ( [REF] ). |
10.1146/annurev.aa.31.090193.002353 | Rowan-Robinson (1977) found that Seyfert 2s have excess dust emission relative to the optical continuum, in comparison with Seyfert is. | found that Seyfert 2s have excess dust emission relative to the optical continuum, in comparison with Seyfert is. | 52 | [
"10.1086/155195"
] | 19,930,101 | [
"1977ApJ...213..635R"
] | [REF] found that Seyfert 2s have excess dust emission relative to the optical continuum, in comparison with Seyfert is. |
10.1146/annurev.aa.31.090193.002353 | This was a wonderful insight, but it seemed inconsistent with the existence of weak featureless continua with low reddening in Seyfert 2s (Koski 1978). | This was a wonderful insight, but it seemed inconsistent with the existence of weak featureless continua with low reddening in Seyfert 2s (). | 55 | [
"10.1086/156235"
] | 19,930,101 | [
"1978ApJ...223...56K"
] | This was a wonderful insight, but it seemed inconsistent with the existence of weak featureless continua with low reddening in Seyfert 2s ([REF]). |
10.1146/annurev.aa.31.090193.002353 | Lawrence & Elvis (1982) derived an elaboration of this picture from an array of statistical correlations among X-ray, narrow line, and broad line emission. | derived an elaboration of this picture from an array of statistical correlations among X-ray, narrow line, and broad line emission. | 56 | [
"10.1086/159918"
] | 19,930,101 | [
"1982ApJ...256..410L"
] | [REF] derived an elaboration of this picture from an array of statistical correlations among X-ray, narrow line, and broad line emission. |
10.1146/annurev.aa.31.090193.002353 | a "Narrow Line Radio Galaxy."1 But Miller and I (Antonucci & Miller 1985) found that the `Osterbrock has called it a Broad Line Radio Galaxy because the broad wings of Ho~ are detectable in total flux. | a "Narrow Line Radio Galaxy."1 But Miller and I () found that the `Osterbrock has called it a Broad Line Radio Galaxy because the broad wings of Ho~ are detectable in total flux. | 76 | [
"10.1086/163559"
] | 19,930,101 | [
"1985ApJ...297..621A"
] | a "Narrow Line Radio Galaxy."1 But Miller and I ([REF]) found that the `Osterbrock has called it a Broad Line Radio Galaxy because the broad wings of Ho~ are detectable in total flux. |
10.1146/annurev.aa.31.090193.002353 | Also as in the case of NGC 1068, the optical spectra were strongly dominated by host galaxy starlight, according to Koski (1978), so that their nuclear continuum polarizations were probably much higher. | Also as in the case of NGC 1068, the optical spectra were strongly dominated by host galaxy starlight, according to , so that their nuclear continuum polarizations were probably much higher. | 100 | [
"10.1086/156235"
] | 19,930,101 | [
"1978ApJ...223...56K"
] | Also as in the case of NGC 1068, the optical spectra were strongly dominated by host galaxy starlight, according to [REF], so that their nuclear continuum polarizations were probably much higher. |
10.1146/annurev.aa.31.090193.002353 | When some of these objects were observed spectropolarimetrically by Miller & Goodrich (1990), they showed broad permitted lines in their polarized flux spectra just like NGC 1068 does. | When some of these objects were observed spectropolarimetrically by , they showed broad permitted lines in their polarized flux spectra just like NGC 1068 does. | 102 | [
"10.1086/168780"
] | 19,930,101 | [
"1990ApJ...355..456M"
] | When some of these objects were observed spectropolarimetrically by [REF], they showed broad permitted lines in their polarized flux spectra just like NGC 1068 does. |
10.1146/annurev.aa.31.090193.002353 | The incredible Z = 2.3 IRAS galaxy F10214+4724 has recently been shown to have 17% broadband optical polarization which could indicate an occulted and reflected quasar or even an occulted and reflected starburst (Lawrence et al 1993). | The incredible Z = 2.3 IRAS galaxy F10214+4724 has recently been shown to have 17% broadband optical polarization which could indicate an occulted and reflected quasar or even an occulted and reflected starburst (). | 137 | [
"10.1093/mnras/260.1.28"
] | 19,930,101 | [
"1993MNRAS.260...28L"
] | The incredible Z = 2.3 IRAS galaxy F10214+4724 has recently been shown to have 17% broadband optical polarization which could indicate an occulted and reflected quasar or even an occulted and reflected starburst ([REF]). |
10.1146/annurev.aa.31.090193.002353 | Similarly, the nuclear IJY spectrum shows absorption by clouds which are opaque at the Lyman limit (Kriss et a! 1992). | Similarly, the nuclear IJY spectrum shows absorption by clouds which are opaque at the Lyman limit (). | 146 | [
"10.1086/171448"
] | 19,930,101 | [
"1992ApJ...392..485K"
] | Similarly, the nuclear IJY spectrum shows absorption by clouds which are opaque at the Lyman limit ([REF]). |
10.1146/annurev.aa.31.090193.002353 | A selection effect such as that described above, and the effect of dynamic range on source size, were both mentioned as possibilities by Ulvestad & Wilson in their 1984 papers. | A selection effect such as that described above, and the effect of dynamic range on source size, were both mentioned as possibilities by . | 158 | [
"10.1086/162520"
] | 19,930,101 | [
"1984ApJ...285..439U"
] | A selection effect such as that described above, and the effect of dynamic range on source size, were both mentioned as possibilities by [REF]. |
10.1146/annurev.aa.31.090193.002353 | These effects were confirmed in studies by Edelson (1987), Ulvestad & Wilson (1989), and Giuricin et al (1990). | These effects were confirmed in studies by , , and . | 159 | [
"10.1086/165004",
"10.1086/167737",
"10.1086/191425"
] | 19,930,101 | [
"1987ApJ...313..651E",
"1989ApJ...343..659U",
"1990ApJS...72..551G"
] | These effects were confirmed in studies by [REF], [REF], and [REF]. |
10.1146/annurev.aa.31.090193.002353 | The SPM model probably does get nailed by the large opening angle suggested by the low polarizations, versus the smaller opening angle derived from the space density of infrared-selected or host-galaxy selected is and 2s (e.g. Lawrence 1991). | The SPM model probably does get nailed by the large opening angle suggested by the low polarizations, versus the smaller opening angle derived from the space density of infrared-selected or host-galaxy selected is and 2s (e.g. ). | 225 | [
"10.1093/mnras/252.4.586"
] | 19,930,101 | [
"1991MNRAS.252..586L"
] | The SPM model probably does get nailed by the large opening angle suggested by the low polarizations, versus the smaller opening angle derived from the space density of infrared-selected or host-galaxy selected is and 2s (e.g. [REF]). |
10.1146/annurev.aa.31.090193.002353 | Morphologically, the blazar JR/optical component is simply the high frequency tail of the radio core emission (e.g. Landau et al 1986, Impey & Neugebauer 1988). | Morphologically, the blazar JR/optical component is simply the high frequency tail of the radio core emission (e.g. ). | 263 | [
"10.1086/164480",
"10.1086/114638"
] | 19,930,101 | [
"1986ApJ...308...78L",
"1988AJ.....95..307I"
] | Morphologically, the blazar JR/optical component is simply the high frequency tail of the radio core emission (e.g. [REF]). |
10.1146/annurev.aa.31.090193.002353 | As expected in this picture, there appear to be no radio quiet blazars (Jannuzi et al 1993a). | As expected in this picture, there appear to be no radio quiet blazars (). | 264 | [
"10.1086/172262"
] | 19,930,101 | [
"1993ApJ...404..100J"
] | As expected in this picture, there appear to be no radio quiet blazars ([REF]). |
10.1146/annurev.aa.31.090193.002353 | That idea, together with the supposedly "normal" emission line equivalent widths (a selection effect I think: Antonucci & Ulvestad 1985) has been used as an argument against optical beaming. | That idea, together with the supposedly "normal" emission line equivalent widths (a selection effect I think: ) has been used as an argument against optical beaming. | 276 | [
"10.1086/163559"
] | 19,930,101 | [
"1985ApJ...297..621A"
] | That idea, together with the supposedly "normal" emission line equivalent widths (a selection effect I think: [REF]) has been used as an argument against optical beaming. |
10.1146/annurev.aa.31.090193.002353 | Modest deviations have been considered by Vagnetti et al (1991). | Modest deviations have been considered by . | 293 | [
"10.1086/169700"
] | 19,930,101 | [
"1991ApJ...368..366V"
] | Modest deviations have been considered by [REF]. |
10.1146/annurev.aa.31.090193.002353 | This prototypical Classical Double NLRG, has a strong nucleus at 2~t (Djorgovski et al 1991), but this is probably dust emission, providing perhaps indirect, but certainly not direct evidence for an obscured quasar. | This prototypical Classical Double NLRG, has a strong nucleus at 2~t (), but this is probably dust emission, providing perhaps indirect, but certainly not direct evidence for an obscured quasar. | 352 | [
"10.1086/186025"
] | 19,930,101 | [
"1991ApJ...372L..67D"
] | This prototypical Classical Double NLRG, has a strong nucleus at 2~t ([REF]), but this is probably dust emission, providing perhaps indirect, but certainly not direct evidence for an obscured quasar. |
10.1146/annurev.aa.31.090193.002353 | The near JR spectrum does not show broad emission lines (Ward et a! 1991), so clearly we aren't seeing the quasar directly just by going to 2~t. | The near JR spectrum does not show broad emission lines (), so clearly we aren't seeing the quasar directly just by going to 2~t. | 353 | [
"10.1086/170699"
] | 19,930,101 | [
"1991ApJ...382..115W"
] | The near JR spectrum does not show broad emission lines ([REF]), so clearly we aren't seeing the quasar directly just by going to 2~t. |
10.1146/annurev.aa.31.090193.002353 | This point was made strongly by Barthel (1989), and resulted in his religious conversion to beaming. | This point was made strongly by , and resulted in his religious conversion to beaming. | 381 | [
"10.1086/167038"
] | 19,930,101 | [
"1989ApJ...336..606B"
] | This point was made strongly by [REF], and resulted in his religious conversion to beaming. |
10.1146/annurev.aa.31.090193.002353 | Garrington et al (1991) added 22 additional jetted sources (with size > 30") to the 25 (with size <30") in Garrington et a! | added 22 additional jetted sources (with size > 30") to the 25 (with size <30") in | 387 | [
"10.1093/mnras/250.1.198"
] | 19,930,101 | [
"1991MNRAS.250..198G"
] | [REF] added 22 additional jetted sources (with size > 30") to the 25 (with size <30") in [REF] |
10.1146/annurev.aa.31.090193.002353 | The Garrington et al (1991) sample is not intended to be complete, but does include most known single-jet objects. | The sample is not intended to be complete, but does include most known single-jet objects. | 390 | [
"10.1093/mnras/250.1.198"
] | 19,930,101 | [
"1991MNRAS.250..198G"
] | The [REF] sample is not intended to be complete, but does include most known single-jet objects. |
10.1146/annurev.aa.31.090193.002353 | This paper, and the companion interpretive one (Garrington & Conway 1991), continue the trend that among objects selected in this way, orientation/beaming effects seem to dominate. | This paper, and the companion interpretive one (), continue the trend that among objects selected in this way, orientation/beaming effects seem to dominate. | 392 | [
"10.1093/mnras/250.1.198"
] | 19,930,101 | [
"1991MNRAS.250..198G"
] | This paper, and the companion interpretive one ([REF]), continue the trend that among objects selected in this way, orientation/beaming effects seem to dominate. |
10.1146/annurev.aa.31.090193.002353 | Heckman (1983) discussed this point, and concluded that the core-dominant and lobe-dominant quasars differed greatly, and that the unified scheme failed. | discussed this point, and concluded that the core-dominant and lobe-dominant quasars differed greatly, and that the unified scheme failed. | 409 | [
"10.1086/184081"
] | 19,930,101 | [
"1983ApJ...271L...5H"
] | [REF] discussed this point, and concluded that the core-dominant and lobe-dominant quasars differed greatly, and that the unified scheme failed. |
10.1146/annurev.aa.31.090193.002353 | The same methodological limitation hinders use of host galaxies for testing the model (Boroson et a! 1985). | The same methodological limitation hinders use of host galaxies for testing the model (). | 416 | [
"10.1086/163219"
] | 19,930,101 | [
"1985ApJ...293..120B"
] | The same methodological limitation hinders use of host galaxies for testing the model ([REF]). |
10.1146/annurev.aa.31.090193.002353 | Various authors (e.g. Lawrence 1991) have found that the [0 III] emission is weaker at a given lobe power in NLRGs compared with broad line radio buds. | Various authors (e.g. ) have found that the [0 III] emission is weaker at a given lobe power in NLRGs compared with broad line radio buds. | 422 | [
"10.1093/mnras/252.4.586"
] | 19,930,101 | [
"1991MNRAS.252..586L"
] | Various authors (e.g. [REF]) have found that the [0 III] emission is weaker at a given lobe power in NLRGs compared with broad line radio buds. |
10.1146/annurev.aa.31.090193.002353 | Prestage & Peacock (1988) came within a factor of a few of matching diffuse radio powers of SSLD and FSCD radio galaxies in their tests, and concluded that the former tend statistically to lie in richer environments than the latter. | came within a factor of a few of matching diffuse radio powers of SSLD and FSCD radio galaxies in their tests, and concluded that the former tend statistically to lie in richer environments than the latter. | 448 | [
"10.1093/mnras/230.1.131"
] | 19,930,101 | [
"1988MNRAS.230..131P"
] | [REF] came within a factor of a few of matching diffuse radio powers of SSLD and FSCD radio galaxies in their tests, and concluded that the former tend statistically to lie in richer environments than the latter. |
10.1146/annurev.aa.31.090193.002353 | Among moderately distant FR 2s, Hutchings (1987) finds that hosts are large and luminous for both the NLRGs and the quasars, with broad 508 ANTONUCCI overlap in their properties, but statistical differences in the means. | Among moderately distant FR 2s, finds that hosts are large and luminous for both the NLRGs and the quasars, with broad 508 ANTONUCCI overlap in their properties, but statistical differences in the means. | 459 | [
"10.1086/165527"
] | 19,930,101 | [
"1987ApJ...320..122H"
] | Among moderately distant FR 2s, [REF] finds that hosts are large and luminous for both the NLRGs and the quasars, with broad 508 ANTONUCCI overlap in their properties, but statistical differences in the means. |
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