source_doi stringclasses 354
values | sent_original stringlengths 39 2.84k | sent_no_cit stringlengths 3 2.8k | sent_idx int64 41 4.59k | citation_dois listlengths 1 7 | pubdate int64 19.8M 20.3M | resolved_bibcodes listlengths 1 7 | sent_cit_masked stringlengths 8 2.81k |
|---|---|---|---|---|---|---|---|
10.1146/annurev.astro.38.1.761 | Fine structure and recombination line ratios imply equivalent “screen” dust extinctions in ULIRGs (and LIRGs) between AV ∼ 5 and 50 ( Genzel et al 1998 ). | Fine structure and recombination line ratios imply equivalent “screen” dust extinctions in ULIRGs (and LIRGs) between AV ∼ 5 and 50 ( ). | 448 | [
"10.1086/305576"
] | 20,000,101 | [
"1998ApJ...498..579G"
] | Fine structure and recombination line ratios imply equivalent “screen” dust extinctions in ULIRGs (and LIRGs) between AV ∼ 5 and 50 ( [REF] ). |
10.1146/annurev.astro.38.1.761 | For radio-quiet QSOs, the sample averaged SEDs of Sanders et al (1989) , Elvis et al (1994) , giving L X /L IR = 0.2 and L X /L bol ∼ 0.05. | For radio-quiet QSOs, the sample averaged SEDs of , giving L X /L IR = 0.2 and L X /L bol ∼ 0.05. | 467 | [
"10.1086/168094",
"10.1086/192093"
] | 20,000,101 | [
"1989ApJ...347...29S",
"1994ApJS...95....1E"
] | For radio-quiet QSOs, the sample averaged SEDs of [REF] , giving L X /L IR = 0.2 and L X /L bol ∼ 0.05. |
10.1146/annurev.astro.38.1.761 | Yet ASCA and BeppoSAX data show that at its center lurks a powerful AGN, attenuated by a Compton thick foreground absorber ( Iwasawa et al 1993 ). | Yet ASCA and BeppoSAX data show that at its center lurks a powerful AGN, attenuated by a Compton thick foreground absorber ( ). | 473 | [
"10.1086/172651"
] | 20,000,101 | [
"1993ApJ...409..155I"
] | Yet ASCA and BeppoSAX data show that at its center lurks a powerful AGN, attenuated by a Compton thick foreground absorber ( [REF] ). |
10.1146/annurev.astro.38.1.761 | A burst may be triggered as the result of the gravitational compression of the gas during the encounters of the nuclei ( Mihos Hernquist 1996 ). | A burst may be triggered as the result of the gravitational compression of the gas during the encounters of the nuclei ( ). | 494 | [
"10.1086/177353"
] | 20,000,101 | [
"1996ApJ...464..641M"
] | A burst may be triggered as the result of the gravitational compression of the gas during the encounters of the nuclei ( [REF] ). |
10.1146/annurev.astro.38.1.761 | Far-IR luminosities of ULIRGs do not change significantly with nuclear separation from separations of a few hundred parsecs to a few tens of kpc ( Rigopoulou et al 1999a ). | Far-IR luminosities of ULIRGs do not change significantly with nuclear separation from separations of a few hundred parsecs to a few tens of kpc ( ). | 499 | [
"10.1086/301146"
] | 20,000,101 | [
"1999AJ....118.2625R"
] | Far-IR luminosities of ULIRGs do not change significantly with nuclear separation from separations of a few hundred parsecs to a few tens of kpc ( [REF] ). |
10.1146/annurev.astro.38.1.761 | <italic>Warm ULIRGs and QSOs</italic> “Warm” ULIRGs (S 25 /S 60 ≥ 0.2) probably represent transition objects between ULIRGs and QSOs ( Sanders et al 1988b ). | <italic>Warm ULIRGs and QSOs</italic> “Warm” ULIRGs (S 25 /S 60 ≥ 0.2) probably represent transition objects between ULIRGs and QSOs ( ). | 500 | [
"10.1086/165983"
] | 20,000,101 | [
"1988ApJ...325...74S"
] | <italic>Warm ULIRGs and QSOs</italic> “Warm” ULIRGs (S 25 /S 60 ≥ 0.2) probably represent transition objects between ULIRGs and QSOs ( [REF] ). |
10.1146/annurev.astro.38.1.761 | This mass is two orders of magnitude greater than the dynamical mass within the central kpc derived from the CO rotation curve ( Downes Solomon 1998 ). | This mass is two orders of magnitude greater than the dynamical mass within the central kpc derived from the CO rotation curve ( ). | 510 | [
"10.1086/306339"
] | 20,000,101 | [
"1998ApJ...507..615D"
] | This mass is two orders of magnitude greater than the dynamical mass within the central kpc derived from the CO rotation curve ( [REF] ). |
10.1146/annurev.astro.38.1.761 | The required mass then is 20 to 100 times smaller, and the ratio of bolometric to K-band luminosity is ≥10 2 ( Thatte et al 1997 ). | The required mass then is 20 to 100 times smaller, and the ratio of bolometric to K-band luminosity is ≥10 2 ( ). | 512 | [
"10.1086/304848"
] | 20,000,101 | [
"1997ApJ...490..238T"
] | The required mass then is 20 to 100 times smaller, and the ratio of bolometric to K-band luminosity is ≥10 2 ( [REF] ). |
10.1146/annurev.astro.38.1.761 | THE DISTANT UNIVERSE In the local Universe surveyed by IRAS, only 30% of the total energy output of galaxies emerges in the mid- and far-IR ( Soifer Neugebauer 1991 ). | THE DISTANT UNIVERSE In the local Universe surveyed by IRAS, only 30% of the total energy output of galaxies emerges in the mid- and far-IR ( ). | 532 | [
"10.1086/115691"
] | 20,000,101 | [
"1991AJ....101..354S"
] | THE DISTANT UNIVERSE In the local Universe surveyed by IRAS, only 30% of the total energy output of galaxies emerges in the mid- and far-IR ( [REF] ). |
10.1146/annurev.astro.38.1.761 | Spectacular (rest frame) UV observations of star-forming galaxies at redshifts ≥3 have become possible in the last few years ( Steidel et al 1996 , Lilly et al 1996 ). | Spectacular (rest frame) UV observations of star-forming galaxies at redshifts ≥3 have become possible in the last few years ( ). | 534 | [
"10.1086/310029",
"10.1086/309975"
] | 20,000,101 | [
"1996ApJ...462L..17S",
"1996ApJ...460L...1L"
] | Spectacular (rest frame) UV observations of star-forming galaxies at redshifts ≥3 have become possible in the last few years ( [REF] ). |
10.1146/annurev.astro.38.1.761 | The inferred star formation rate per (comoving) volume element increases from z = 0 by more than an order of magnitude to a peak at z ∼ 1–3 ( Madau et al 1996 , Pettini et al 1998 , Steidel et al 1999 ). | The inferred star formation rate per (comoving) volume element increases from z = 0 by more than an order of magnitude to a peak at z ∼ 1–3 ( ). | 535 | [
"10.1093/mnras/283.4.1388",
"10.1086/306431",
"10.1086/307363"
] | 20,000,101 | [
"1996MNRAS.283.1388M",
"1998ApJ...508..539P",
"1999ApJ...519....1S"
] | The inferred star formation rate per (comoving) volume element increases from z = 0 by more than an order of magnitude to a peak at z ∼ 1–3 ( [REF] ). |
10.1146/annurev.astro.38.1.761 | <italic>Source Counts: Evidence for Strong Evolution</italic> Figure 14 (from Serjeant, private communication; Elbaz et al 1999a ) gives the integrated and differential source counts derived from these surveys. | <italic>Source Counts: Evidence for Strong Evolution</italic> Figure 14 (from ) gives the integrated and differential source counts derived from these surveys. | 564 | [
"10.48550/arXiv.astro-ph/9910406"
] | 20,000,101 | [
"1999A&A...351L..37E"
] | <italic>Source Counts: Evidence for Strong Evolution</italic> Figure 14 (from [REF] ) gives the integrated and differential source counts derived from these surveys. |
10.1146/annurev.astro.38.1.761 | The interpretation of the bump is that with luminosity evolution and flat or even “negative” k-correction (between z = 0.5 and 1; Elbaz et al 1999b ) the number counts increase initially, with decreasing flux density much faster than Euclidean. | The interpretation of the bump is that with luminosity evolution and flat or even “negative” k-correction (between z = 0.5 and 1; ) the number counts increase initially, with decreasing flux density much faster than Euclidean. | 588 | [
"10.48550/arXiv.astro-ph/9910406"
] | 20,000,101 | [
"1999A&A...351L..37E"
] | The interpretation of the bump is that with luminosity evolution and flat or even “negative” k-correction (between z = 0.5 and 1; [REF] ) the number counts increase initially, with decreasing flux density much faster than Euclidean. |
10.1146/annurev.astro.38.1.761 | In contrast, the pure density evolution model predicts a much smaller median redshift (∼0.5) and essentially no sources with z > 1. When the mid-infrared counts are compared to K-band counts at the same energy (νS ν ), the mid-infrared sources contribute only about 10% of the energy at the bright end, but more than 50%... | In contrast, the pure density evolution model predicts a much smaller median redshift (∼0.5) and essentially no sources with z > 1. When the mid-infrared counts are compared to K-band counts at the same energy (νS ν ), the mid-infrared sources contribute only about 10% of the energy at the bright end, but more than 50%... | 590 | [
"10.48550/arXiv.astro-ph/9910406"
] | 20,000,101 | [
"1999A&A...351L..37E"
] | In contrast, the pure density evolution model predicts a much smaller median redshift (∼0.5) and essentially no sources with z > 1. When the mid-infrared counts are compared to K-band counts at the same energy (νS ν ), the mid-infrared sources contribute only about 10% of the energy at the bright end, but more than 50%... |
10.1146/annurev.astro.38.1.761 | In the (10′) 2 CFRS 1415+52 field, Flores et al (1999b) detected 78 significant (≥3σ) 15 μm sources (≥250 μJy), 22 of which have spectra and redshifts. | In the (10′) 2 CFRS 1415+52 field, detected 78 significant (≥3σ) 15 μm sources (≥250 μJy), 22 of which have spectra and redshifts. | 601 | [
"10.1086/307172"
] | 20,000,101 | [
"1999ApJ...517..148F"
] | In the (10′) 2 CFRS 1415+52 field, [REF] detected 78 significant (≥3σ) 15 μm sources (≥250 μJy), 22 of which have spectra and redshifts. |
10.1146/annurev.astro.38.1.761 | For 19 galaxies with complete radio to UV SEDs, Flores et al (1999b) identified more than half as (highly reddened) starbursts. | For 19 galaxies with complete radio to UV SEDs, identified more than half as (highly reddened) starbursts. | 612 | [
"10.1086/307172"
] | 20,000,101 | [
"1999ApJ...517..148F"
] | For 19 galaxies with complete radio to UV SEDs, [REF] identified more than half as (highly reddened) starbursts. |
10.1146/annurev.astro.38.1.761 | Rigopoulou et al (1999b) have recently carried out near-IR, VLT-ISAAC spectroscopy of a sample of 0.6 ≤ z ≤ 1.3 ISOCAM galaxies in the HDF(S) field. | have recently carried out near-IR, VLT-ISAAC spectroscopy of a sample of 0.6 ≤ z ≤ 1.3 ISOCAM galaxies in the HDF(S) field. | 616 | [
"10.1086/301146"
] | 20,000,101 | [
"1999AJ....118.2625R"
] | [REF] have recently carried out near-IR, VLT-ISAAC spectroscopy of a sample of 0.6 ≤ z ≤ 1.3 ISOCAM galaxies in the HDF(S) field. |
10.1146/annurev.astro.38.1.761 | For HDF(s) Rigopoulou et al 2000 and Franceschini 2000 (private communication) deduced star formation rates of a few tens of M yr −1 from the Hα emission but typically three times greater values from the mid-IR data. | For HDF(s) and deduced star formation rates of a few tens of M yr −1 from the Hα emission but typically three times greater values from the mid-IR data. | 622 | [
"10.48550/arXiv.astro-ph/9912544"
] | 20,000,101 | [
"2000LNP...548..240R"
] | For HDF(s) [REF] and [REF] deduced star formation rates of a few tens of M yr −1 from the Hα emission but typically three times greater values from the mid-IR data. |
10.1146/annurev.astro.38.1.761 | A smaller fraction (∼25%) of the CFRS sources have ULIRG-like luminosities (10 12 L), in agreement with the work of Rowan-Robinson et al (1997) for HDF(N). | A smaller fraction (∼25%) of the CFRS sources have ULIRG-like luminosities (10 12 L), in agreement with the work of for HDF(N). | 624 | [
"10.1093/mnras/289.2.490"
] | 20,000,101 | [
"1997MNRAS.289..490R"
] | A smaller fraction (∼25%) of the CFRS sources have ULIRG-like luminosities (10 12 L), in agreement with the work of [REF] for HDF(N). |
10.1146/annurev.astro.38.1.761 | (a) galaxies in Coma, only those with emission lines have excess mid-IR emission indicative of active star formation ( Quillen et al 1999 ). | (a) galaxies in Coma, only those with emission lines have excess mid-IR emission indicative of active star formation ( ). | 629 | [
"10.1086/307307"
] | 20,000,101 | [
"1999ApJ...518..632Q"
] | (a) galaxies in Coma, only those with emission lines have excess mid-IR emission indicative of active star formation ( [REF] ). |
10.1146/annurev.astro.38.1.761 | Flores et al (1999a) identified 40% of the 15 CFRS/6.75 μm galaxies with spectra as AGNs, and 53% as active starbursts or S+A galaxies. | identified 40% of the 15 CFRS/6.75 μm galaxies with spectra as AGNs, and 53% as active starbursts or S+A galaxies. | 631 | [
"10.1086/307172"
] | 20,000,101 | [
"1999ApJ...517..148F"
] | [REF] identified 40% of the 15 CFRS/6.75 μm galaxies with spectra as AGNs, and 53% as active starbursts or S+A galaxies. |
10.1146/annurev.astro.38.1.761 | The hatched upper limits in the mid-IR are derived from the lack of attenuation of high-energy γ-rays ( Hauser et al 1998 ). | The hatched upper limits in the mid-IR are derived from the lack of attenuation of high-energy γ-rays ( ). | 647 | [
"10.1086/306379"
] | 20,000,101 | [
"1998ApJ...508...25H"
] | The hatched upper limits in the mid-IR are derived from the lack of attenuation of high-energy γ-rays ( [REF] ). |
10.1146/annurev.astro.38.1.761 | In the best areas, the surveys are limited by the fluctuations in the extragalactic background ( Lagache Puget 1999 ). | In the best areas, the surveys are limited by the fluctuations in the extragalactic background ( ). | 658 | [
"10.48550/arXiv.astro-ph/9901059"
] | 20,000,101 | [
"1999A&A...344..322L"
] | In the best areas, the surveys are limited by the fluctuations in the extragalactic background ( [REF] ). |
10.1146/annurev.astro.38.1.761 | The interplay of the k-corrections is such that ISOCAM cannot see galaxies with an Arp 220 SED located at z ∼ 2. The integrated counts constitute less than 10% of the COBE far-IR background ( Hauser et al 1998 ). | The interplay of the k-corrections is such that ISOCAM cannot see galaxies with an Arp 220 SED located at z ∼ 2. The integrated counts constitute less than 10% of the COBE far-IR background ( ). | 681 | [
"10.1086/306379"
] | 20,000,101 | [
"1998ApJ...508...25H"
] | The interplay of the k-corrections is such that ISOCAM cannot see galaxies with an Arp 220 SED located at z ∼ 2. The integrated counts constitute less than 10% of the COBE far-IR background ( [REF] ). |
10.1146/annurev.astro.38.1.761 | Star Formation at High Redshift: A Synthesis From the survey of the 1415+52 CFRS field, Flores et al (1999b) concluded that 60 ± 25% of the star formation at z ≤ 1 is associated with infrared emission. | Star Formation at High Redshift: A Synthesis From the survey of the 1415+52 CFRS field, concluded that 60 ± 25% of the star formation at z ≤ 1 is associated with infrared emission. | 684 | [
"10.1086/307172"
] | 20,000,101 | [
"1999ApJ...517..148F"
] | Star Formation at High Redshift: A Synthesis From the survey of the 1415+52 CFRS field, [REF] concluded that 60 ± 25% of the star formation at z ≤ 1 is associated with infrared emission. |
10.1146/annurev.astro.38.1.761 | Rowan-Robinson et al (1997) found an even larger correction factor from an analysis of the ISOCAM HDF(N) data. | found an even larger correction factor from an analysis of the ISOCAM HDF(N) data. | 686 | [
"10.1093/mnras/289.2.490"
] | 20,000,101 | [
"1997MNRAS.289..490R"
] | [REF] found an even larger correction factor from an analysis of the ISOCAM HDF(N) data. |
10.1146/annurev.astro.38.1.761 | Finally, the 850 μm source detections with the SCUBA bolometer camera require a star formation rate at z ∼ 3 that is ∼3.5 times greater than that derived from Lyman-dropout galaxies ( Hughes et al 1998 , Barger et al 1998 , Ivison et al 1998 ). | Finally, the 850 μm source detections with the SCUBA bolometer camera require a star formation rate at z ∼ 3 that is ∼3.5 times greater than that derived from Lyman-dropout galaxies ( ). | 688 | [
"10.1038/28328",
"10.1038/28338",
"10.1046/j.1365-8711.1998.01677.x"
] | 20,000,101 | [
"1998Natur.394..241H",
"1998Natur.394..248B",
"1998MNRAS.298..583I"
] | Finally, the 850 μm source detections with the SCUBA bolometer camera require a star formation rate at z ∼ 3 that is ∼3.5 times greater than that derived from Lyman-dropout galaxies ( [REF] ). |
10.1146/annurev.astro.38.1.761 | To explain the entire COBE far-IR/submm background requires that the star formation rate at z ≥ 1 be greater by another factor ≥2 ( Lagache et al 1999b ). | To explain the entire COBE far-IR/submm background requires that the star formation rate at z ≥ 1 be greater by another factor ≥2 ( ). | 690 | [
"10.48550/arXiv.astro-ph/9901059"
] | 20,000,101 | [
"1999A&A...344..322L"
] | To explain the entire COBE far-IR/submm background requires that the star formation rate at z ≥ 1 be greater by another factor ≥2 ( [REF] ). |
10.1146/annurev.astro.38.1.761 | The large discrepancy between the UV and IR/submm estimates disappears if the star formation rates estimated from the Lyman-dropout galaxies are corrected for extinction ( Pettini et al 1998 , Meurer et al 1999 , Steidel et al 1999 ). | The large discrepancy between the UV and IR/submm estimates disappears if the star formation rates estimated from the Lyman-dropout galaxies are corrected for extinction ( ). | 692 | [
"10.1086/306431",
"10.1086/307523",
"10.1086/307363"
] | 20,000,101 | [
"1998ApJ...508..539P",
"1999ApJ...521...64M",
"1999ApJ...519....1S"
] | The large discrepancy between the UV and IR/submm estimates disappears if the star formation rates estimated from the Lyman-dropout galaxies are corrected for extinction ( [REF] ). |
10.1146/annurev.astro.38.1.761 | The black symbols (with error bars) denote the star formation history deduced from (non-extinction corrected) UV data ( Steidel et al 1999 and references therein). | The black symbols (with error bars) denote the star formation history deduced from (non-extinction corrected) UV data ( and references therein). | 695 | [
"10.1086/307363"
] | 20,000,101 | [
"1999ApJ...519....1S"
] | The black symbols (with error bars) denote the star formation history deduced from (non-extinction corrected) UV data ( [REF] and references therein). |
10.1146/annurev.astro.38.1.761 | The red, three arrow symbol denotes the lower limit to dusty star formation obtained from SCUBA observations of HDF (N) ( Hughes et al 1998 ). | The red, three arrow symbol denotes the lower limit to dusty star formation obtained from SCUBA observations of HDF (N) ( ). | 698 | [
"10.1038/28328"
] | 20,000,101 | [
"1998Natur.394..241H"
] | The red, three arrow symbol denotes the lower limit to dusty star formation obtained from SCUBA observations of HDF (N) ( [REF] ). |
10.1146/annurev.astro.38.1.761 | The continuous line marks the total star formation rate deduced from the COBE background and an ‘inversion’ with a starburt SED ( Lagache et al 1999b ). | The continuous line marks the total star formation rate deduced from the COBE background and an ‘inversion’ with a starburt SED ( ). | 699 | [
"10.48550/arXiv.astro-ph/9901059"
] | 20,000,101 | [
"1999A&A...344..322L"
] | The continuous line marks the total star formation rate deduced from the COBE background and an ‘inversion’ with a starburt SED ( [REF] ). |
10.1146/annurev.astro.38.1.761 | Based on the X-ray background, Almaini et al (1999) set a limit of ∼20% to the AGN contribution to the far-IR/submm background. | Based on the X-ray background, set a limit of ∼20% to the AGN contribution to the far-IR/submm background. | 708 | [
"10.1046/j.1365-8711.1999.02669.x"
] | 20,000,101 | [
"1999MNRAS.305L..59A"
] | Based on the X-ray background, [REF] set a limit of ∼20% to the AGN contribution to the far-IR/submm background. |
10.1146/annurev.astro.38.1.761 | A rapidly evolving “burst” mode (exhaust time scales a few hundred Myrs) is required, probably associated with the much increased merger rate at high redshift [∝ (1 + z) δ , δ=2..6; Zepf Koo 1989 , Carlberg 1990 , Abraham et al 1996 ]. | A rapidly evolving “burst” mode (exhaust time scales a few hundred Myrs) is required, probably associated with the much increased merger rate at high redshift [∝ (1 + z) δ , δ=2..6; ]. | 715 | [
"10.1086/167085",
"10.1086/185782",
"10.1093/mnras/279.3.L47"
] | 20,000,101 | [
"1989ApJ...337...34Z",
"1990ApJ...359L...1C",
"1996MNRAS.279L..47A"
] | A rapidly evolving “burst” mode (exhaust time scales a few hundred Myrs) is required, probably associated with the much increased merger rate at high redshift [∝ (1 + z) δ , δ=2..6; [REF] ]. |
10.1146/annurev.astro.38.1.761 | The ultraluminous mergers may be related to the formation of large elliptical galaxies and bulges ( Kormendy Sanders 1992 ). | The ultraluminous mergers may be related to the formation of large elliptical galaxies and bulges ( ). | 724 | [
"10.1086/186370"
] | 20,000,101 | [
"1992ApJ...390L..53K"
] | The ultraluminous mergers may be related to the formation of large elliptical galaxies and bulges ( [REF] ). |
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