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Título de Acceso Abierto
The Astrophysical Journal (ApJ)
Resumen/Descripción – provisto por la editorial en inglés
The Astrophysical Journal is an open access journal devoted to recent developments, discoveries, and theories in astronomy and astrophysics. Publications in ApJ constitute significant new research that is directly relevant to astrophysical applications, whether based on observational results or on theoretical insights or modeling.Palabras clave – provistas por la editorial
astronomy; astrophysics
Disponibilidad
| Institución detectada | Período | Navegá | Descargá | Solicitá |
|---|---|---|---|---|
| No detectada | desde jul. 1995 / hasta dic. 2023 | IOPScience |
Información
Tipo de recurso:
revistas
ISSN impreso
0004-637X
ISSN electrónico
1538-4357
Editor responsable
American Astronomical Society (AAS)
Idiomas de la publicación
- inglés
País de edición
Reino Unido
Información sobre licencias CC
Cobertura temática
Tabla de contenidos
NuSTARHARD X-RAY SURVEY OF THE GALACTIC CENTER REGION. I. HARD X-RAY MORPHOLOGY AND SPECTROSCOPY OF THE DIFFUSE EMISSION
Kaya Mori
; Charles J. Hailey; Roman Krivonos; Jaesub Hong; Gabriele Ponti; Franz Bauer; Kerstin Perez; Melania Nynka; Shuo Zhang; John A. Tomsick; David M. Alexander; Frederick K. Baganoff; Didier Barret; Nicolas Barrière; Steven E. Boggs; Alicia M. Canipe; Finn E. Christensen; William W. Craig; Karl Forster; Paolo Giommi; Brian W. Grefenstette; Jonathan E. Grindlay; Fiona A. Harrison; Allan Hornstrup; Takao Kitaguchi; Jason E. Koglin; Vy Luu; Kristen K. Madsen; Peter H. Mao; Hiromasa Miyasaka; Matteo Perri; Michael J. Pivovaroff; Simonetta Puccetti; Vikram Rana; Daniel Stern; Niels J. Westergaard; William W. Zhang; Andreas Zoglauer
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 94
AN INCREASING STELLAR BARYON FRACTION IN BRIGHT GALAXIES AT HIGH REDSHIFT
Steven L. Finkelstein; Mimi Song; Peter Behroozi; Rachel S. Somerville; Casey Papovich; Miloš Milosavljević; Avishai Dekel; Desika Narayanan; Matthew L. N. Ashby; Asantha Cooray; Giovanni G. Fazio; Henry C. Ferguson; Anton M. Koekemoer; Brett Salmon; S. P. Willner
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 95
EXCITATION MECHANISMS FOR HCN(1–0) AND HCO+(1–0) IN GALAXIES FROM THE GREAT OBSERVATORIES ALL-SKY LIRG SURVEY*
G. C. Privon; R. Herrero-Illana; A. S. Evans; K. Iwasawa; M. A. Perez-Torres; L. Armus; T. Díaz-Santos; E. J. Murphy; S. Stierwalt; S. Aalto; J. M. Mazzarella; L. Barcos-Muñoz; H. J. Borish; H. Inami; D.-C. Kim; E. Treister; J. A. Surace; S. Lord; J. Conway; D. T. Frayer; A. Alberdi
<jats:title>ABSTRACT</jats:title> <jats:p>We present new Institut de Radioastronomie Millimétrique (IRAM) 30 m spectroscopic observations of the ∼88 GHz band, including emission from the <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{CCH}(N=1\to 0)$?> </jats:tex-math> <?MML <mml:math> <mml:mi>CCH</mml:mi> <mml:mspace width="0.50em"/> <mml:mo stretchy="true">(</mml:mo> <mml:mi>N</mml:mi> <mml:mo>=</mml:mo> <mml:mn>1</mml:mn> <mml:mo>→</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true">)</mml:mo> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn1.gif" xlink:type="simple" /> </jats:inline-formula> multiplet, HCN (<jats:inline-formula> <jats:tex-math> <?CDATA $J=1\to 0)$?> </jats:tex-math> <?MML <mml:math> <mml:mi>J</mml:mi> <mml:mo>=</mml:mo> <mml:mn>1</mml:mn> <mml:mo>→</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true">)</mml:mo> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn2.gif" xlink:type="simple" /> </jats:inline-formula>, <jats:inline-formula> <jats:tex-math> <?CDATA ${\mathrm{HCO}}^{+}(J=1\to 0)$?> </jats:tex-math> <?MML <mml:math> <mml:msup> <mml:mrow> <mml:mi>HCO</mml:mi> </mml:mrow> <mml:mrow> <mml:mo form="prefix">+</mml:mo> </mml:mrow> </mml:msup> <mml:mspace width="0.50em"/> <mml:mo stretchy="true">(</mml:mo> <mml:mi>J</mml:mi> <mml:mo>=</mml:mo> <mml:mn>1</mml:mn> <mml:mo>→</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true">)</mml:mo> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn3.gif" xlink:type="simple" /> </jats:inline-formula>, and <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{HNC}(J=1\to 0)$?> </jats:tex-math> <?MML <mml:math> <mml:mi>HNC</mml:mi> <mml:mspace width="0.50em"/> <mml:mo stretchy="true">(</mml:mo> <mml:mi>J</mml:mi> <mml:mo>=</mml:mo> <mml:mn>1</mml:mn> <mml:mo>→</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true">)</mml:mo> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn4.gif" xlink:type="simple" /> </jats:inline-formula>, for a sample of 58 local luminous and ultraluminous infrared galaxies from the Great Observatories All-sky LIRG Survey (GOALS). By combining our new IRAM data with literature data and <jats:italic>Spitzer</jats:italic>/IRS spectroscopy, we study the correspondence between these putative tracers of dense gas and the relative contribution of active galactic nuclei (AGNs) and star formation to the mid-infrared luminosity of each system. We find the HCN (1–0) emission to be enhanced in AGN-dominated systems (<jats:inline-formula> <jats:tex-math> <?CDATA $\langle $?> </jats:tex-math> <?MML <mml:math> <mml:mo stretchy="true">⟨</mml:mo> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn5.gif" xlink:type="simple" /> </jats:inline-formula> <jats:inline-formula> <jats:tex-math> <?CDATA ${L}_{\mathrm{HCN}(1-0)}^{\prime }$?> </jats:tex-math> <?MML <mml:math> <mml:msubsup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>HCN</mml:mi> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mn>1</mml:mn> <mml:mo form="prefix">–</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true" form="prefix">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mo accent="true" form="prefix">′</mml:mo> </mml:mrow> </mml:msubsup> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn6.gif" xlink:type="simple" /> </jats:inline-formula>/<jats:inline-formula> <jats:tex-math> <?CDATA ${L}_{{\mathrm{HCO}}^{+}(1-0)}^{\prime }$?> </jats:tex-math> <?MML <mml:math> <mml:msubsup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow> <mml:mi>HCO</mml:mi> </mml:mrow> <mml:mrow> <mml:mo form="prefix">+</mml:mo> </mml:mrow> </mml:msup> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mn>1</mml:mn> <mml:mo form="prefix">–</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true" form="prefix">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mo accent="true" form="prefix">′</mml:mo> </mml:mrow> </mml:msubsup> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn7.gif" xlink:type="simple" /> </jats:inline-formula> <jats:inline-formula> <jats:tex-math> <?CDATA $\rangle =1.84$?> </jats:tex-math> <?MML <mml:math> <mml:mo stretchy="true">⟩</mml:mo> <mml:mo>=</mml:mo> <mml:mn>1.84</mml:mn> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn8.gif" xlink:type="simple" /> </jats:inline-formula>), compared to composite and starburst-dominated systems (<jats:inline-formula> <jats:tex-math> <?CDATA $\langle $?> </jats:tex-math> <?MML <mml:math> <mml:mo stretchy="true">⟨</mml:mo> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn9.gif" xlink:type="simple" /> </jats:inline-formula> <jats:inline-formula> <jats:tex-math> <?CDATA ${L}_{\mathrm{HCN}(1-0)}^{\prime }$?> </jats:tex-math> <?MML <mml:math> <mml:msubsup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>HCN</mml:mi> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mn>1</mml:mn> <mml:mo form="prefix">–</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true" form="prefix">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mo accent="true" form="prefix">′</mml:mo> </mml:mrow> </mml:msubsup> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn10.gif" xlink:type="simple" /> </jats:inline-formula>/<jats:inline-formula> <jats:tex-math> <?CDATA ${L}_{{\mathrm{HCO}}^{+}(1-0)}^{\prime }$?> </jats:tex-math> <?MML <mml:math> <mml:msubsup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow> <mml:mi>HCO</mml:mi> </mml:mrow> <mml:mrow> <mml:mo form="prefix">+</mml:mo> </mml:mrow> </mml:msup> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mn>1</mml:mn> <mml:mo form="prefix">–</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true" form="prefix">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mo accent="true" form="prefix">′</mml:mo> </mml:mrow> </mml:msubsup> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn11.gif" xlink:type="simple" /> </jats:inline-formula> <jats:inline-formula> <jats:tex-math> <?CDATA $\rangle \;=1.14,$?> </jats:tex-math> <?MML <mml:math> <mml:mo stretchy="true">⟩</mml:mo> <mml:mspace width="0.25em"/> <mml:mo>=</mml:mo> <mml:mn>1.14</mml:mn> <mml:mo>,</mml:mo> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn12.gif" xlink:type="simple" /> </jats:inline-formula> and 0.88, respectively). However, some composite and starburst systems have <jats:inline-formula> <jats:tex-math> <?CDATA ${L}_{\mathrm{HCN}(1-0)}^{\prime }$?> </jats:tex-math> <?MML <mml:math> <mml:msubsup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>HCN</mml:mi> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mn>1</mml:mn> <mml:mo form="prefix">–</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true" form="prefix">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mo accent="true" form="prefix">′</mml:mo> </mml:mrow> </mml:msubsup> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn13.gif" xlink:type="simple" /> </jats:inline-formula>/<jats:inline-formula> <jats:tex-math> <?CDATA ${L}_{{\mathrm{HCO}}^{+}(1-0)}^{\prime }$?> </jats:tex-math> <?MML <mml:math> <mml:msubsup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow> <mml:mi>HCO</mml:mi> </mml:mrow> <mml:mrow> <mml:mo form="prefix">+</mml:mo> </mml:mrow> </mml:msup> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mn>1</mml:mn> <mml:mo form="prefix">–</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true" form="prefix">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mo accent="true" form="prefix">′</mml:mo> </mml:mrow> </mml:msubsup> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn14.gif" xlink:type="simple" /> </jats:inline-formula> ratios comparable to those of AGNs, indicating that enhanced HCN emission is not uniquely associated with energetically dominant AGNs. After removing AGN-dominated systems from the sample, we find a linear relationship (within the uncertainties) between log<jats:sub>10</jats:sub>(<jats:inline-formula> <jats:tex-math> <?CDATA ${L}_{\mathrm{HCN}(1-0)}^{\prime }$?> </jats:tex-math> <?MML <mml:math> <mml:msubsup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>HCN</mml:mi> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mn>1</mml:mn> <mml:mo form="prefix">–</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true" form="prefix">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mo accent="true" form="prefix">′</mml:mo> </mml:mrow> </mml:msubsup> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn15.gif" xlink:type="simple" /> </jats:inline-formula>) and log<jats:sub>10</jats:sub>(<jats:italic>L</jats:italic> <jats:sub>IR</jats:sub>), consistent with most previous findings. <jats:inline-formula> <jats:tex-math> <?CDATA ${L}_{\mathrm{HCN}(1-0)}^{\prime }$?> </jats:tex-math> <?MML <mml:math> <mml:msubsup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>HCN</mml:mi> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mn>1</mml:mn> <mml:mo form="prefix">–</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true" form="prefix">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mo accent="true" form="prefix">′</mml:mo> </mml:mrow> </mml:msubsup> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn16.gif" xlink:type="simple" /> </jats:inline-formula>/<jats:italic>L</jats:italic> <jats:sub>IR</jats:sub>, typically interpreted as the dense-gas depletion time, appears to have no systematic trend with <jats:italic>L</jats:italic> <jats:sub>IR</jats:sub> for our sample of luminous and ultraluminous infrared galaxies, and has significant scatter. The galaxy-integrated <jats:inline-formula> <jats:tex-math> <?CDATA ${L}_{\mathrm{HCN}(1-0)}^{\prime }$?> </jats:tex-math> <?MML <mml:math> <mml:msubsup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>HCN</mml:mi> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mn>1</mml:mn> <mml:mo form="prefix">–</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true" form="prefix">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mo accent="true" form="prefix">′</mml:mo> </mml:mrow> </mml:msubsup> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn17.gif" xlink:type="simple" /> </jats:inline-formula> and <jats:inline-formula> <jats:tex-math> <?CDATA ${L}_{{\mathrm{HCO}}^{+}(1-0)}^{\prime }$?> </jats:tex-math> <?MML <mml:math> <mml:msubsup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow> <mml:mi>HCO</mml:mi> </mml:mrow> <mml:mrow> <mml:mo form="prefix">+</mml:mo> </mml:mrow> </mml:msup> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mn>1</mml:mn> <mml:mo form="prefix">–</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true" form="prefix">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mo accent="true" form="prefix">′</mml:mo> </mml:mrow> </mml:msubsup> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apj520621ieqn18.gif" xlink:type="simple" /> </jats:inline-formula> emission do not appear to have a simple interpretation in terms of the AGN dominance or the star formation rate, and are likely determined by multiple processes, including density and radiative effects.</jats:p>
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 39
THE STAR FORMATION HISTORY OF BCGs TOz= 1.8 FROM THE SpARCS/SWIRE SURVEY: EVIDENCE FOR SIGNIFICANT IN SITU STAR FORMATION AT HIGH REDSHIFT
Tracy M. A. Webb; Adam Muzzin; Allison Noble; Nina Bonaventura; James Geach; Yashar Hezevah; Chris Lidman; Gillian Wilson; H. K. C. Yee; Jason Surace; David Shupe
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 96
A MULTIWAVELENGTH STUDY OF TADPOLE GALAXIES IN THE HUBBLE ULTRA DEEP FIELD
Amber N. Straughn; Elysse N. Voyer; Rafael T. Eufrasio; Duilia de Mello; Sara Petty; Susan Kassin; Jonathan P. Gardner; Swara Ravindranath; Emmaris Soto
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 97
FORMATION OF RAMAN SCATTERING WINGS AROUND Hα, Hβ, AND PAαIN ACTIVE GALACTIC NUCLEI
Seok-Jun Chang; Jeong-Eun Heo; Francesco Di Mille; Rodolfo Angeloni; Tali Palma; Hee-Won Lee
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 98
FROM SOLAR TO STELLAR CORONA: THE ROLE OF WIND, ROTATION, AND MAGNETISM
Victor Réville; Allan Sacha Brun; Antoine Strugarek; Sean P. Matt; Jérôme Bouvier; Colin P. Folsom; Pascal Petit
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 99
ON HELIUM 1083 nm LINE POLARIZATION DURING THE IMPULSIVE PHASE OF AN X1 FLARE
Philip G. Judge; Lucia Kleint; Alberto Sainz Dalda
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 100
THE HIGH-VELOCITY SYSTEM: INFALL OF A GIANT LOW-SURFACE-BRIGHTNESS GALAXY TOWARD THE CENTER OF THE PERSEUS CLUSTER
Alice P.-Y. Yu; Jeremy Lim; Youichi Ohyama; Jeffrey C.-C. Chan; T. Broadhurst
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 101
RAYLEIGH SCATTERING IN THE ATMOSPHERE OF THE WARM EXO-NEPTUNE GJ 3470B
Diana Dragomir; Björn Benneke; Kyle A. Pearson; Ian J. M. Crossfield; Jason Eastman; Travis Barman; Lauren I. Biddle
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 102