bluuebunny/crossref_metadata_2025_split huggingface dataset:
Candidate Water Vapor Lines to Locate the H2O Snowline Through High-dispersion Spectroscopic Observations. II. The Case of a Herbig Ae Star
Authors: Notsu Shota , Nomura Hideko , Ishimoto Daiki , Walsh Catherine , Honda Mitsuhiko , Hirota Tomoya , Millar T. J. 
Published: February 2017

Abstract
Observationally measuring the location of the

H

2

O

snowline is crucial for understanding planetesimal and planet formation processes, and the origin of water on Earth. In disks around Herbig Ae stars (T
* ∼ 10,000 K, M
* ≳ 2.5M
⊙), the position of the

H

2

O

snowline is farther from the central star compared with that around cooler and less massive T Tauri stars. Thus, the

H

2

O

emission line fluxes from the region within the

H

2

O

snowline are expected to be stronger. In this paper, we calculate the chemical composition of a Herbig Ae disk using chemical kinetics. Next, we calculate the

H

2

O

emission line profiles and investigate the properties of candidate water lines across a wide range of wavelengths (from mid-infrared to submillimeter) that can locate the position of the

H

2

O

snowline. Those lines identified have small Einstein A coefficients (

∼

10

−
6

–

10

−
3

s−1) and relatively high upper-state energies (∼1000 K). The total fluxes tend to increase with decreasing wavelengths. We investigate the possibility of future observations (e.g., ALMA, SPICA/SMI-HRS) locating the position of the

H

2

O

snowline. Since the fluxes of those identified lines from Herbig Ae disks are stronger than those from T Tauri disks, the possibility of a successful detection is expected to increase for a Herbig Ae disk.
The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ∼106 L⊙ and Comparisons with Galaxy Formation Models
Authors: Roediger Joel C. , Ferrarese Laura , Côté Patrick , MacArthur Lauren A. , Sánchez-Janssen Rúben , Blakeslee John P. , Peng Eric W. , Liu Chengze , Munoz Roberto , Cuillandre Jean-Charles , Gwyn Stephen , Mei Simona , Boissier Samuel , Boselli Alessandro , Cantiello Michele , Courteau Stéphane , Duc Pierre-Alain , Lançon Ariane , Mihos J. Christopher , Puzia Thomas H. , Taylor James E. , Durrell Patrick R. , Toloba Elisa , Guhathakurta Puragra , Zhang Hongxin 
Published: February 2017

Abstract
We use deep optical photometry from the Next Generation Virgo Cluster Survey (NGVS) to investigate the color–magnitude diagram for the galaxies inhabiting the core of this cluster. The sensitivity of the NGVS imaging allows us to continuously probe galaxy colors over a factor of ∼2 × 105 in luminosity, from brightest cluster galaxies to scales overlapping classical satellites of the Milky Way (

M

g
′

∼ −9; M
* ∼ 106
M
⊙), within a single environment. Remarkably, we find the first evidence that the red sequence (RS) flattens in all colors at the faint-magnitude end (starting between −14 ≤

M

g
′

≤ −13, around M
* ∼ 4 × 107
M
⊙), with the slope decreasing to ∼60% or less of its value at brighter magnitudes. This could indicate that the stellar populations of faint dwarfs in Virgo’s core share similar characteristics (e.g., constant mean age) over ∼3 mag in luminosity, suggesting that these galaxies were quenched coevally, likely via pre-processing in smaller hosts. We also compare our results to galaxy formation models, finding that the RS in model clusters have slopes at intermediate magnitudes that are too shallow, and in the case of semianalytic models, do not reproduce the flattening seen at both extremes (bright/faint) of the Virgo RS. Deficiencies in the chemical evolution of model galaxies likely contribute to the model-data discrepancies at all masses, while overly efficient quenching may also be a factor at dwarf scales. Deep UV and near-IR photometry are required to unambiguously diagnose the cause of the faint-end flattening.
Magnetic Separatrix as the Source Region of the Plasma Supply for an Active-region Filament
Authors: Zou P. , Fang C. , Chen P. F. , Yang K. , Cao Wenda 
Published: February 2017

Abstract
Solar filaments can be formed via chromospheric evaporation followed by condensation in the corona or by the direct injection of cool plasma from the chromosphere to the corona. We here confirm with high-resolution Hα data observed by the 1.6 m New Solar Telescope of the Big Bear Solar Observatory on 2015 August 21 that an active-region filament is maintained by the continuous injection of cold chromospheric plasma. We find that the filament is rooted along a bright ridge in Hα, which corresponds to the intersection of a magnetic quasi-separatrix layer with the solar surface. This bright ridge consists of many small patches whose sizes are comparable to the width of the filament threads. It is found that upflows originate from the brighter patches of the ridge, whereas the downflows move toward the weaker patches of the ridge. The whole filament is composed of two opposite-direction streams, implying that longitudinal oscillations are not the only cause of the counterstreamings, and unidirectional siphon flows with alternative directions are another possibility.
CO-Dark Star Formation and Black Hole Activity in 3C 368 at z = 1.131: Coeval Growth of Stellar and Supermassive Black Hole Masses∗
†
Authors: Lamarche C. , Stacey G. , Brisbin D. , Ferkinhoff C. , Hailey-Dunsheath S. , Nikola T. , Riechers D. , Sharon C. E. , Spoon H. , Vishwas A. 
Published: February 2017

Abstract
We present the detection of four far-infrared fine-structure oxygen lines, as well as strong upper limits for the CO(2–1) and [N ii] 205 μm lines, in 3C 368, a well-studied radio-loud galaxy at z = 1.131. These new oxygen lines, taken in conjunction with previously observed neon and carbon fine-structure lines, suggest a powerful active galactic nucleus (AGN), accompanied by vigorous and extended star formation. A starburst dominated by O8 stars, with an age of ∼6.5 Myr, provides a good fit to the fine-structure line data. This estimated age of the starburst makes it nearly concurrent with the latest episode of AGN activity, suggesting a link between the growth of the supermassive black hole and stellar population in this source. We do not detect the CO(2–1) line, down to a level twelve times lower than the expected value for star-forming galaxies. This lack of CO line emission is consistent with recent star formation activity if the star-forming molecular gas has low metallicity, is highly fractionated (such that CO is photodissociated throughout much of the clouds), or is chemically very young (such that CO has not yet had time to form). It is also possible, although we argue it is unlikely, that the ensemble of fine-structure lines is emitted from the region heated by the AGN.
Discovery and Precise Characterization by the MEarth Project of LP 661-13, an Eclipsing Binary Consisting of Two Fully Convective Low-mass Stars
Authors: Dittmann Jason A. , Irwin Jonathan M. , Charbonneau David , Berta-Thompson Zachory K. , Newton Elisabeth R. , Latham David W. , Latham Christian A. , Esquerdo Gilbert , Berlind Perry , Calkins Michael L 
Published: February 2017

Abstract
We report the detection of stellar eclipses in the LP 661-13 system. We present the discovery and characterization of this system, including high-resolution spectroscopic radial velocities and a photometric solution spanning two observing seasons. LP 661-13 is a low-mass binary system with an orbital period of

days at a distance of 24.9 ± 1.3 parsecs. LP 661-13A is a 0.30795 ± 0.00084 M
⊙ star, while LP 661-13B is a 0.19400 ± 0.00034 M
⊙ star. The radius of each component is 0.3226 ± 0.0033 R
⊙ and 0.2174 ± 0.0023 R
⊙, respectively. We detect out-of-eclipse modulations at a period slightly shorter than the orbital period, implying that at least one of the components is not rotating synchronously. We find that each component is slightly inflated compared to stellar models, and that this cannot be reconciled through age or metallicity effects. As a nearby eclipsing binary system, where both components are near or below the full-convection limit, LP 661-13 will be a valuable test of models for the structure of cool dwarf stars.
Planck Lensing and Cosmic Infrared Background Cross-correlation with Fermi-LAT: Tracing Dark Matter Signals in the Gamma-Ray Background
Authors: Feng Chang , Cooray Asantha , Keating Brian 
Published: February 2017

Abstract
The extragalactic γ-ray background and its spatial anisotropy could potentially contain a signature of dark matter (DM) annihilation or particle decay. Astrophysical foregrounds, such as blazars and star-forming galaxies (SFGs), however, dominate the γ-ray background, precluding an easy detection of the signal associated with the DM annihilation or decay in the background intensity spectrum. The DM imprint on the γ-ray background is expected to be correlated with large-scale structure tracers. In some cases, such a cross-correlation is even expected to have a higher signal-to-noise ratio than the auto-correlation. One reliable tracer of the DM distribution in the large-scale structure is lensing of the cosmic microwave background (CMB), and the cosmic infrared background (CIB) is a reliable tracer of SFGs. We analyze Fermi-LAT data taken over 92 months and study the cross-correlation with Planck CMB lensing, Planck CIB, and Fermi-γ maps. We put upper limits on the DM annihilation cross-section from the cross-power spectra with the γ-ray background anisotropies. The unbiased power spectrum estimation is validated with simulations that include cross-correlated signals. We also provide a set of systematic tests and show that no significant contaminations are found for the measurements presented here. Using γ-ray background map from data gathered over 92 months, we find the best constraint on the DM annihilation with a

1
σ

confidence level upper limit of 10−25–10−24 cm3 s−1, when the mass of DM particles is between 20 and 100 GeV.
Constraining the Stellar Populations and Star Formation Histories of Blue Compact Dwarf Galaxies with SED Fits
Authors: Janowiecki Steven , Salzer John J. , Zee Liese van , Rosenberg Jessica L. , Skillman Evan 
Published: February 2017

Abstract
We discuss and test possible evolutionary connections between blue compact dwarf galaxies (BCDs) and other types of dwarf galaxies. BCDs provide ideal laboratories to study intense star formation episodes in low-mass dwarf galaxies, and have sometimes been considered a short-lived evolutionary stage between types of dwarf galaxies. To test these connections, we consider a sample of BCDs as well as a comparison sample of nearby galaxies from the Local Volume Legacy (LVL) survey for context. We fit the multi-wavelength spectral energy distributions (SED, far-ultra-violet to far-infrared) of each galaxy with a grid of theoretical models to determine their stellar masses and star formation properties. We compare our results for BCDs with the LVL galaxies to put BCDs in the context of normal galaxy evolution. The SED fits demonstrate that the star formation events currently underway in BCDs are at the extreme of the continuum of normal dwarf galaxies, both in terms of the relative mass involved and in the relative increase over previous star formation rates. Today’s BCDs are distinctive objects in a state of extreme star formation that is rapidly transforming them. This study also suggests ways to identify former BCDs whose star formation episodes have since faded.
The Dependence of Cluster Galaxy Properties on the Central Entropy of Their Host Cluster
Authors: Kim Jae-Woo , Ko Jongwan , Hwang Ho Seong , Edge Alastair C. , Lee Joon Hyeop , Lee Jong Chul , Jeong Hyunjin 
Published: February 2017

Abstract
We present a study of the connection between brightest cluster galaxies (BCGs) and their host galaxy clusters. Using galaxy clusters at

from the Hectospec Cluster Survey (HeCS) with X-ray information from the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT), we confirm that BCGs in low central entropy clusters are well aligned with the X-ray center. Additionally, the magnitude difference between BCG and the second brightest galaxy also correlates with the central entropy of the intracluster medium. From the red-sequence (RS) galaxies, we cannot find significant dependence of RS color scatter and stellar population on the central entropy of the intracluster medium of their host cluster. However, BCGs in low-entropy clusters are systematically less massive than those in high-entropy clusters, although this is dependent on the method used to derive the stellar mass of BCGs. In contrast, the stellar velocity dispersion of BCGs shows no dependence on BCG activity and cluster central entropy. This implies that the potential of the BCG is established earlier and the activity leading to optical emission lines is dictated by the properties of the intracluster medium in the cluster core.
Fundamental Plane of Black Hole Activity in the Quiescent Regime
Authors: Xie Fu-Guo , Yuan Feng 
Published: February 2017

Abstract
A correlation among the radio luminosity (

L

R

), X-ray luminosity (

L

X

), and black hole (BH) mass (

M

BH

) in active galactic nuclei (AGNs) and BH binaries is known to exist and is called the “fundamental plane” of BH activity. Yuan & Cui predict that the radio/X-ray correlation index,

ξ

X

, changes from

ξ

X

≈
0.6

to

ξ

X

≈
1.2
–
1.3

when

L

X

/

L

Edd

decreases below a critical value of

∼

10

−
6

. While many works favor such a change, there are also several works claiming the opposite. In this paper, we gather from the literature the largest quiescent AGN (defined as

L

X

/

L

Edd

≲

10

−
6

) sample to date, consisting of 75 sources. We find that these quiescent AGNs follow a

ξ

X

≈
1.23

radio/X-ray relationship, in excellent agreement with the Yuan & Cui prediction. The reason for the discrepancy between the present result and some previous works is that their samples contain not only quiescent sources but also “normal” ones (i.e.,

L

X

/

L

Edd

≳

10

−
6

). In this case, the quiescent sources will mix up with those normal ones in

L

R

and

L

X

. The value of

ξ

X

will then be between 0.6 and ∼1.3, with the exact value being determined by the sample composition, i.e., the fraction of the quiescent and normal sources. Based on this result, we propose that a more physical way to study the fundamental plane is to replace

L

R

and

L

X

with

L

R

/

L

Edd

and

L

X

/

L

Edd

, respectively.
Evolutions and Calibrations of Long Gamma-Ray-burst Luminosity Correlations Revisited
Authors: Wang Guo-Jian , Yu Hai , Li Zheng-Xiang , Xia Jun-Qing , Zhu Zong-Hong 
Published: February 2017

Abstract
Luminosity correlations of long gamma-ray bursts (GRBs) are extensively proposed as an effective complementarity to trace the Hubble diagram of the universe at high redshifts, which is of great importance to explore properties of dark energy. Recently, several empirical luminosity correlations have been statistically proposed from GRB observations. However, to treat a GRB as the distance indicator, there are two key issues: the redshift evolution of luminosity correlations and their calibrations. In this paper, we choose the Amati relation, the correlation between the peak spectra energy and the equivalent isotropic energy of GRBs (

E

p

–

E

iso

) as an example and find that the current GRB data set implies that there could be a evolution of the luminosity correlation with respect to the redshift. Therefore, we propose an extended Amati relation with two extra redshift-dependent terms to correct the redshift evolution of the GRB relation. Second, we carefully check the reliability of the calibration method using the low-redshift GRB data. Importantly, we find that the low-redshift calibration method does not take whole correlations between

Ω

m

and coefficients into account. Neglecting this correlation information can break the degeneracies and obtain the biased constraint on

Ω

m

, which is very sensitive to values of parameters for the calibration. A small shift in the parameters of the “calibrated” relation could significantly change the final constraint on

Ω

m

in the low-redshift calibration method. Finally, we simulate several GRB samples with different statistical errors and find that, in order to correctly recover the fiducial value of

Ω

m

, using the low-redshift calibration method, we need a large number of GRB samples with high precisions.
The Effects of the Overshooting of the Convective Core on Main-sequence Turnoffs of Young- and Intermediate-age Star Clusters
Authors: Yang Wuming , Tian Zhijia 
Published: February 2017

Abstract
Recent investigations have shown that the extended main-sequence turnoffs (eMSTOs) are a common feature of intermediate-age star clusters in the Magellanic Clouds. The eMSTOs are also found in the color–magnitude diagram of young-age star clusters. The origin of the eMSTOs is still an open question. Moreover, asteroseismology shows that the value of the overshooting parameter

of the convective core is not fixed for the stars with an approximatelly equal mass. Thus the MSTO of star clusters may be affected by the overshooting of the convective core (OVCC). We calculated the effects of the OVCC with different δ
ov on the MSTO of young- and intermediate-age star clusters. If δ
ov varies between stars in a cluster, the observed eMSTOs of young- and intermediate-age star clusters can be explained well by the effects. The equivalent age spreads of MSTO caused by the OVCC are related to the age of star clusters and are in good agreement with observed results of many clusters. Moreover, the observed eMSTOs of NGC 1856 are reproduced by the coeval populations with different δ
ov. The eMSTOs of star clusters may be relevant to the effects of the OVCC. The effects of the OVCC are similar to that of rotation in some respects. However, the effects cannot result in a significant split of the main sequence of young star clusters at

. The presence of a rapid rotation can make the split of the main sequence of young star clusters more significant.
Laser-Assisted Capsulotomy Centration: A Prospective Trial Comparing Pupil Versus OCT-Based Scanned Capsule Centration
Authors: Schultz Tim , Tsiampalis Nikolaos , Dick H. Burkhard 
Published: February 2017

PURPOSE:
To investigate different capsulotomy centration methods for femtosecond laser-assisted cataract surgery. The overlap between intraocular lens (IOL) optic and lens capsule was measured with different centration methods and IOL types.

METHODS:
This was a prospective randomized clinical trial. Patients with cataract scheduled for femtosecond laser-assisted cataract surgery were assigned to one of four treatment groups: optical coherence tomography (OCT)-based scanned capsule centration (SCC) and three-piece IOL (SCC with three-piece IOL); scanned capsule centration and plate-haptic IOL (SCC with plate-haptic IOL); pupil centration (PC) and three-piece IOL (PC with three-piece IOL); or PC and plate-haptic IOL (PC with plate-haptic IOL). At the end of surgery, the overlap between the IOL optic and capsular bag was measured.

RESULTS:

The results of 160 patients were evaluated (n = 40 in each group). There was no difference in age (
P
= .27), sex (
P
= .18), the number of treated left and right eyes (
P
= .64), or cataract grade (
P
= .06). With the new SCC method (capsulotomy diameter: 5 mm), a complete overlap was achieved in all cases in both SCC groups. The overlap was also complete in all cases with PC and plate-haptic IOLs. In the PC with three-piece IOL group, the overlap was incomplete in 3 eyes.

CONCLUSIONS:
The SCC method helps to achieve a 360° overlap in all eyes independent of the IOL type. A complete 360° overlap was achieved in all cases up to a calculated capsulotomy diameter of 5.1 mm with this new method.

[
J Refract Surg
. 2017;33(2):74–78.]
Life-history data for the funnel weavers Eratigena agrestis and Eratigena atrica (Araneae: Agelenidae) in the Pacific Northwest of North America
Authors: Vibert Samantha , Salomon Maxence , Scott Catherine , Blackburn Gwylim S. , Gries Gerhard 
Published: February 2017

AbstractThe life history of the funnel weaver Eratigena agrestis (Walckenaer) (Araneae: Agelenidae) is not well studied despite its widespread occurrence in Europe and its establishment and spread in the Pacific Northwest of North America since its introduction in the early 20th century. We report phenology and life-history data for E. agrestis and another co-occurring funnel weaver, Eratigena atrica (Koch), in two study sites in British Columbia, Canada. The most notable difference in phenology between the two Eratigena species was the timing of emergence: E. atrica spiderlings emerge in the fall whereas E. agrestis spiderlings emerge in the spring. Surprisingly, the contrasting densities of E. atrica in the two study sites and the presence of the western black widow spider, Latrodectus hesperus Chamberlin and Ivie (Araneae: Theridiidae), in one study site had little effect on the life history of E. agrestis. This unexpected finding may be explained by (i) low overall competition pressure in the study habitats, (ii) conspecifics and heterospecifics exerting equivalent competition or predation pressures; and/or (iii) aggregations of heterospecifics providing benefits that offset costs associated with any competition.
Nitrate radicals and biogenic volatile organic compounds: oxidation, mechanisms, and organic aerosol
Authors: Ng Nga Lee , Brown Steven S. , Archibald Alexander T. , Atlas Elliot , Cohen Ronald C. , Crowley John N. , Day Douglas A. , Donahue Neil M. , Fry Juliane L. , Fuchs Hendrik , Griffin Robert J. , Guzman Marcelo I. , Herrmann Hartmut , Hodzic Alma , Iinuma Yoshiteru , Jimenez José L. , Kiendler-Scharr Astrid , Lee Ben H. , Luecken Deborah J. , Mao Jingqiu , McLaren Robert , Mutzel Anke , Osthoff Hans D. , Ouyang Bin , Picquet-Varrault Benedicte , Platt Ulrich , Pye Havala O. T. , Rudich Yinon , Schwantes Rebecca H. , Shiraiwa Manabu , Stutz Jochen , Thornton Joel A. , Tilgner Andreas , Williams Brent J. , Zaveri Rahul A. 
Published: February 2017

Abstract. Oxidation of biogenic volatile organic compounds (BVOC) by the nitrate radical (NO3) represents one of the important interactions between anthropogenic emissions related to combustion and natural emissions from the biosphere. This interaction has been recognized for more than 3 decades, during which time a large body of research has emerged from laboratory, field, and modeling studies. NO3-BVOC reactions influence air quality, climate and visibility through regional and global budgets for reactive nitrogen (particularly organic nitrates), ozone, and organic aerosol. Despite its long history of research and the significance of this topic in atmospheric chemistry, a number of important uncertainties remain. These include an incomplete understanding of the rates, mechanisms, and organic aerosol yields for NO3-BVOC reactions, lack of constraints on the role of heterogeneous oxidative processes associated with the NO3 radical, the difficulty of characterizing the spatial distributions of BVOC and NO3 within the poorly mixed nocturnal atmosphere, and the challenge of constructing appropriate boundary layer schemes and non-photochemical mechanisms for use in state-of-the-art chemical transport and chemistry–climate models. This review is the result of a workshop of the same title held at the Georgia Institute of Technology in June 2015. The first half of the review summarizes the current literature on NO3-BVOC chemistry, with a particular focus on recent advances in instrumentation and models, and in organic nitrate and secondary organic aerosol (SOA) formation chemistry. Building on this current understanding, the second half of the review outlines impacts of NO3-BVOC chemistry on air quality and climate, and suggests critical research needs to better constrain this interaction to improve the predictive capabilities of atmospheric models.