bluuebunny/crossref_metadata_2025_split huggingface dataset:
THE EFFECT OF LEADERSHIP STYLE ON QUALITY OF SERVICE THROUGH ORGANIZATIONAL CULTURE IN THE DEPARTMENT OF INVESTMENT, ESDM, AND TRANSMIGRATION OF GORONTALO PROVINCE
Authors: Abbas Syahrawanty S. , Wantu Sastro Mustapa 
Published: March 2023

<p>This research was conducted with the aim of analyzing the Influence of Leadership Style on Service Quality Through Organizational Culture in the Investment Office, ESDM and Transmigration of Gorontalo Province. This research uses descriptive type of quantitative approach by measuring the influence of the variable leadership style on service quality through organizational culture. The results showed that the leadership style variable showed a value of 3.092 with a significance value of 0.003 &lt;0.05. The value of t table is 1,984. Thus, obtained t-count 3.092 &gt; 1.984 which means that the hypothesis which states that leadership style has a positive and significant effect on service quality is accepted. The t-count value for the organizational culture variable shows the t-count value = 6.668 with a significance value of 0.000 &lt;0.05. The value of t table is 1,984. Thus, obtained t-count (6.668) &gt; t-table (1.984) which means that the hypothesis which states that organizational culture has a positive and significant influence on service quality can be accepted. The significance value of the leadership style variable on organizational culture is0.00&lt;0.05 with a t-count value of 8.649 and t-table is1.984 or 8.649 &gt; 1.98. This means that there is a significant influence of the leadership style variable on organizational culture.</p>
Reticulocyte Count and Platelet Count as Predictors of Morphological Remission/Hemopoitic Recovery in Acute Lymphoblastic Leukemia (ALL) after Induction Chemotherapy
Authors: Huma Riaz, Hamzullah Khan, Shahtaj Khan, Sadaf Chiragh  
Published: March 2023

Objectives: To determine the predictive values of reticulocyte and platelet count for remission in cases of acute lymphoblastic leukemia after induction therapy.

Materials and Methods:This cross-sectional observational study was conducted in the department of hematology, MTI Hayatabad Medical Complex, Peshawar. All cases of ALL referred to the department for remission after taking induction therapy, irrespective of age and gender were included. Relevant information wascollected on a predesigned proforma prepared in accordance with the objectives of the study.

Results: A total of 84 cases referred for remission were included, 56(66.7%) were males and 28 (33.3%) were females. 50(59.5%) cases were in the age range of 5-18 years. The mean with a standard deviation of the age of patients was 15+ 4 years. 75(89.3%) of the cases were classified into ALL-1) by FAB classification. 50(59.5%) of the referred cases had achieved morphological remission by bone marrow aspiration. There was a statistically significant rise in Platelet count of the remission vs non-remission cases (p-0.001). Again there was a statistically significant difference in the retic count of the cases with remission (p-0.05). We observed a statically significant downhill moderate correlation ofretic count with remission (in termsof blast count of BM aspiration) (p-0.04, r:-0.32). Platelet count also had an inverse significant correlation with remission ( p-0.01, r:-0.37). The diagnostic roles of the peripheral platelet count and retic yielded an area under curves of (0.768 and 0.648 respectively) to predict remission.We observed that the retic count and platelet count havebeen shown to have strong predictive valuesfor remission in ALL with interaction values of (R= 0.28**, ΔR²=0.02, p=0.08). Similarly, an increase in platelet also has a strong predictive value for remission in ALL cases with interaction values of (R= 0.41**, ΔR²=0.16, p=0.001)

Conclusion: In ALL cases of post-induction therapy, The peripheral blood reading for an increase in Retic and platelet count predictsremission with 95% confidence. These values if strictly observed can reduce the frequency of invasive procedures like bone marrow aspiration.

Keywords: ALL, Remission, Reticulocyte count, Platelet count.
A Survey of Herbig Ae/Be Multiplicity
Authors: Thomas S. J. , Rodgers B. , van der Bliek N. S. , Doppmann G. , Bouvier J. , Salvo C. Araya , Beuzit J.-L. , Rigaut F. 
Published: March 2023

Abstract
Although the majority of Herbig Ae/Be (HAEBE) stars are likely multiple systems, relatively few multiples have been identified. We aim to create a statistically significant survey of HAEBE multiplicity as a function of stellar mass, to shed light on mixed-mass star formation. Two independent adaptive optics IR imaging surveys were conducted, between 1993 and 2007. A total of 143 stars were observed, including 126 HAEBE stars. These surveys are significantly more sensitive than previous imaging work and, combined with accurate distance and proper-motion data from GAIA Data Release 3, provide a broad survey of intermediate-mass multiplicity. We perform a statistical probability analysis to identify the likely physical companions, and analyze multiepoch observations for common proper motions. We find 250 stellar detections around 88 sample stars. Of these, 70 systems are likely multiple systems, and 42 companions around 29 systems are reported here for the first time. Correcting for completeness, we find a multiplicity fraction of 54%. Multiples are found randomly across all spectral types, but high-order multiples are more common among the hottest stars. Statistically likely companions are found at distances of up to several thousand astronomical units and ΔK magnitudes ranging from <0.1 to ∼9, although companions with ΔK < 1.5 are rare. Companions around Herbig Ae stars tend to be closer than those around Herbig Be stars. We confirm 24 proper-motion companions in 21 systems, including roughly half of the statistically very likely companions; however, many proper-motion results are inconclusive.
Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Tokovinin Andrei 
Published: March 2023

Abstract
New spectroscopic orbits of inner subsystems in 14 hierarchies are determined from long-term monitoring with the optical echelle spectrometer, CHIRON. Their main components are nearby solar-type stars belonging to nine triple systems (HIP 3645, 14307, 36165, 79980, 103735, 103814, 104440, 105879, 109443) and five quadruples of 2 + 2 hierarchy (HIP 41171, 49336, 75663, 78163, and 117666). The inner periods range from 254 days to 18 yr. Inner subsystems in HIP 3645, 14313, 79979, 103735, 104440, and 105879 are resolved by speckle interferometry, and their combined spectro-interferometric orbits are derived here. Astrometric orbits of HIP 49336 Aa,Ab and HIP 117666 Aa,Ab are determined from wobble in the observed motion of the outer pairs. Comparison with three spectroscopic orbits found in the Gaia data release 3 archive reveals that Gaia underestimated the amplitudes (except for HIP 109443), while the periods match approximately. This work contributes new data on the architecture of nearby hierarchical systems, complementing their statistics.
Evidence for AGN-regulated Cooling in Clusters at z ∼ 1.4: A Multiwavelength View of SPT-CL J0607-4448
Authors: Masterson Megan , McDonald Michael , Ansarinejad Behzad , Bayliss Matthew , Benson Bradford A. , Bleem Lindsey E. , Calzadilla Michael S. , Edge Alastair C. , Floyd Benjamin , Kim Keunho J. , Khullar Gourav , Somboonpanyakul Taweewat 
Published: March 2023

Abstract
We present a multiwavelength analysis of the galaxy cluster SPT-CL J0607-4448 (SPT0607), which is one of the most distant clusters discovered by the South Pole Telescope at z = 1.4010 ± 0.0028. The high-redshift cluster shows clear signs of being relaxed with well-regulated feedback from the active galactic nucleus (AGN) in the brightest cluster galaxy (BCG). Using Chandra X-ray data, we construct thermodynamic profiles and determine the properties of the intracluster medium. The cool-core nature of the cluster is supported by a centrally peaked density profile and low central entropy (

K

0

=

18

−
9

+
11

keV cm2), which we estimate assuming an isothermal temperature profile due to the limited spectral information given the distance to the cluster. Using the density profile and gas cooling time inferred from the X-ray data, we find a mass-cooling rate

M

̇

cool

=

100

−
60

+
90

M

⊙

yr−1. From optical spectroscopy and photometry around the [O ii] emission line, we estimate that the BCG star formation rate is

SFR

[
O

II
]

=

1.7

−
0.6

+
1.0

M

⊙

yr−1, roughly two orders of magnitude lower than the predicted mass-cooling rate. In addition, using ATCA radio data at 2.1 GHz, we measure a radio jet power

P

cav

=

3.2

−
1.3

+
2.1

×

10

44

erg s−1, which is consistent with the X-ray cooling luminosity (

L

cool

=

1.9

−
0.5

+
0.2

×

10

44

erg s−1 within r
cool = 43 kpc). These findings suggest that SPT0607 is a relaxed, cool-core cluster with AGN-regulated cooling at an epoch shortly after cluster formation, implying that the balance between cooling and feedback can be reached quickly. We discuss the implications for these findings on the evolution of AGN feedback in galaxy clusters.
ALMA Lensing Cluster Survey: Properties of Millimeter Galaxies Hosting X-Ray-detected Active Galactic Nuclei
Authors: Uematsu Ryosuke , Ueda Yoshihiro , Kohno Kotaro , Yamada Satoshi , Toba Yoshiki , Fujimoto Seiji , Hatsukade Bunyo , Umehata Hideki , Espada Daniel , Sun Fengwu , Magdis Georgios E. , Kokorev Vasily , Ao Yiping 
Published: March 2023

Abstract
We report the multiwavelength properties of millimeter galaxies hosting X-ray detected active galactic nuclei (AGNs) from the ALMA Lensing Cluster Survey (ALCS). ALCS is an extensive survey of well-studied lensing clusters with ALMA, covering an area of 133 arcmin2 over 33 clusters with a 1.2 mm flux-density limit of ∼60 μJy (1σ). Utilizing the archival data of Chandra, we identify three AGNs at z = 1.06, 2.09, and 2.84 among the 180 millimeter sources securely detected in the ALCS (of which 155 are inside the coverage of Chandra). The X-ray spectral analysis shows that two AGNs are not significantly absorbed (

log

N

H

/

cm

−
2

<
23

), while the other shows signs of moderate absorption (

log

N

H

/

cm

−
2

∼
23.5

). We also perform spectral energy distribution modeling of X-ray to millimeter photometry. We find that our X-ray AGN sample shows both high mass-accretion rates (intrinsic 0.5–8 keV X-ray luminosities of ∼1044–45 erg s−1) and star formation rates (≳100 M
⊙ yr−1). This demonstrates that a wide-area survey with ALMA and Chandra can selectively detect intense growth of both galaxies and supermassive black holes in the high-redshift universe.
JWST/NIRCam Probes Young Star Clusters in the Reionization Era
Sunrise Arc
Authors: Vanzella Eros , Claeyssens Adélaïde , Welch Brian , Adamo Angela , Coe Dan , Diego Jose M. , Mahler Guillaume , Khullar Gourav , Kokorev Vasily , Oguri Masamune , Ravindranath Swara , Furtak Lukas J. , Hsiao Tiger Yu-Yang , Abdurro’uf  , Mandelker Nir , Brammer Gabriel , Bradley Larry D. , Bradač Maruša , Conselice Christopher J. , Dayal Pratika , Nonino Mario , Andrade-Santos Felipe , Windhorst Rogier A. , Pirzkal Nor , Sharon Keren , de Mink S. E. , Fujimoto Seiji , Zitrin Adi , Eldridge Jan J. , Norman Colin 
Published: March 2023

Abstract
Star cluster formation in the early universe and its contribution to reionization
remains largely unconstrained to date. Here we present JWST/NIRCam imaging of
the most highly magnified galaxy known at z ∼ 6,
the Sunrise arc. We identify six young massive star
clusters (YMCs) with measured radii spanning from ∼20 down to ∼1 pc (corrected
for lensing magnification), estimated stellar masses of ∼106–7
M
⊙, and ages of 1–30 Myr based on SED fitting to photometry measured
in eight filters extending to rest frame 7000 Å. The resulting stellar mass
surface densities are higher than 1000 M
⊙ pc−2 (up to a few 105
M
⊙ pc−2), and their inferred dynamical ages qualify the
majority of these systems as gravitationally bound stellar clusters. The star
cluster ages map the progression of star formation along the arc, with two
evolved systems (≳10 Myr old) followed by very young clusters. The youngest
stellar clusters (<5 Myr) show evidence of prominent Hβ+[O iii] emission based on photometry with equivalent
widths larger than >1000 Å rest frame and are hosted in a 200 pc sized
star-forming complex. Such a region dominates the ionizing photon production
with a high efficiency

log
(

ξ

ion

[
Hz

erg

−
1

]
)
∼
25.7

. A significant fraction of the recently formed stellar mass of
the galaxy (10%–30%) occurred in these YMCs. We speculate that such sources of
ionizing radiation boost the ionizing photon production efficiency, which
eventually carves ionized channels that might favor the escape of Lyman
continuum radiation. The survival of some of the clusters would make them the
progenitors of massive and relatively metal-poor globular clusters in the local
universe.
First Observations of the Brown Dwarf HD 19467 B with JWST
Authors: Greenbaum Alexandra Z. , Llop-Sayson Jorge , Lew Ben W.P. , Bryden Geoffrey , Roellig Thomas L. , Ygouf Marie , Fulton B. J. , Hey Daniel R. , Huber Daniel , Mukherjee Sagnick , Meyer Michael , Leisenring Jarron , Rieke Marcia , Boyer Martha , Green Joseph J. , Kelly Doug , Misselt Karl , Serabyn Eugene , Stansberry John , Chu Laurie E. U. , De Furio Matthew , Johnstone Doug , Schlieder Joshua E. , Beichman Charles 
Published: March 2023

Abstract
We observed HD 19467 B with JWST’s NIRCam in six filters spanning 2.5–4.6 μm with the long-wavelength bar coronagraph. The brown dwarf HD 19467 B was initially identified through a long-period trend in the radial velocity of the G3V star HD 19467. HD 19467 B was subsequently detected via coronagraphic imaging and spectroscopy, and characterized as a late-T type brown dwarf with an approximate temperature ∼1000 K. We observed HD 19467 B as a part of the NIRCam GTO science program, demonstrating the first use of the NIRCam Long Wavelength Bar coronagraphic mask. The object was detected in all six filters (contrast levels of 2 × 10−4 to 2 × 10−5) at a separation of 1.″6 using angular differential imaging and synthetic reference differential imaging. Due to a guide star failure during the acquisition of a preselected reference star, no reference star data were available for post-processing. However, reference differential imaging was successfully applied using synthetic point-spread functions developed from contemporaneous maps of the telescope’s optical configuration. Additional radial velocity data (from Keck/HIRES) are used to constrain the orbit of HD 19467 B. Photometric data from TESS are used to constrain the properties of the host star, particularly its age. NIRCam photometry, spectra, and photometry from the literature, and improved stellar parameters are used in conjunction with recent spectral and evolutionary substellar models to derive the physical properties of HD 19467 B. Using an age of 9.4 ± 0.9 Gyr inferred from spectroscopy, Gaia astrometry, and TESS asteroseismology, we obtain a model-derived mass of 62 ± 1 M
J, which is consistent within 2σ with the dynamically derived mass of

81

−
12

+
14

M
J.
A Catalog of 71 Coronal Line Galaxies in MaNGA: [Ne v] Is an Effective AGN Tracer
Authors: Negus James , Comerford Julia M. , Sánchez Francisco Müller , Revalski Mitchell , Riffel Rogemar A. , Bundy Kevin , Nevin Rebecca , Rembold Sandro B. 
Published: March 2023

Abstract
Despite the importance of active galactic nuclei (AGNs) in galaxy evolution, accurate AGN identification is often challenging, as common AGN diagnostics can be confused by contributions from star formation and other effects (e.g., Baldwin–Phillips–Terlevich diagrams). However, one promising avenue for identifying AGNs is “coronal emission lines” (“CLs”), which are highly ionized species of gas with ionization potentials ≥100 eV. These CLs may serve as excellent signatures for the strong ionizing continuum of AGNs. To determine if CLs are in fact strong AGN tracers, we assemble and analyze the largest catalog of optical CL galaxies using the Sloan Digital Sky Survey's Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) catalog. We detect CL emission in 71 MaNGA galaxies, out of the 10,010 unique galaxies from the final MaNGA catalog, with ≥5σ confidence. In our sample, we measure [Ne v]λ3347, λ3427, [Fe vii]λ3586, λ3760, λ6086, and [Fe x]λ6374 emission and crossmatch the CL galaxies with a catalog of AGNs that were confirmed with broad-line, X-ray, IR, and radio observations. We find that [Ne v] emission, compared to [Fe vii] and [Fe x] emission, is best at identifying high-luminosity AGNs. Moreover, we find that the CL galaxies with the least dust extinction yield the most iron CL detections. We posit that the bulk of the iron CLs are destroyed by dust grains in the galaxies with the highest [O iii] luminosities in our sample, and that AGNs in the galaxies with low [O iii] luminosities are possibly too weak to be detected using traditional techniques.
A Broadband X-Ray Study of the Rabbit Pulsar Wind Nebula Powered by PSR J1418-6058
Authors: Park Jaegeun , Kim Chanho , Woo Jooyun , An Hongjun , Mori Kaya , Reynolds Stephen P. , Safi-Harb Samar 
Published: March 2023

Abstract
We report on broadband X-ray properties of the Rabbit pulsar wind nebula (PWN) associated with the pulsar PSR J1418−6058 using archival Chandra and XMM-Newton data, as well as a new NuSTAR observation. NuSTAR data above 10 keV allowed us to detect the 110 ms spin period of the pulsar, characterize its hard X-ray pulse profile, and resolve hard X-ray emission from the PWN after removing contamination from the pulsar and other overlapping point sources. The extended PWN was detected up to ∼20 keV and is described well by a power-law model with a photon index Γ ≈ 2. The PWN shape does not vary significantly with energy, and its X-ray spectrum shows no clear evidence of softening away from the pulsar. We modeled the spatial profile of X-ray spectra and broadband spectral energy distribution in the radio to TeV band to infer the physical properties of the PWN. We found that a model with low magnetic field strength (B ∼ 10 μG) and efficient diffusion (D ∼ 1027 cm2 s−1) fits the PWN data well. The extended hard X-ray and TeV emission, associated respectively with synchrotron radiation and inverse Compton scattering by relativistic electrons, suggest that particles are accelerated to very high energies (≳500 TeV), indicating that the Rabbit PWN is a Galactic PeVatron candidate.
Extinction of Taurus, Orion, Perseus, and California Molecular Clouds Based on the LAMOST, 2MASS, and Gaia Surveys. I. 3D Extinction and Structure
Authors: Cao 曹 ZheTai 哲泰 , Jiang 姜 Biwei 碧沩 , Zhao 赵 He 赫 , Sun 孙 Mingxu 明旭 
Published: March 2023

Abstract
The 3D extinction and structure are studied for the Taurus, Orion, Perseus, and California molecular clouds based on the LAMOST spectroscopy. Stellar color excess is calculated with the intrinsic color index derived from the atmospheric parameters in the LAMOST DR8 catalog and the observed color index in the Gaia EDR3 and the 2MASS PSC. In combination with the distance from the Gaia EDR3 parallax, the 3D dust extinction maps are retrieved in the color excesses

E

G

BP

,

G

RP

and

E

J
,

K

S

with an uncertainty of ∼0.03 mag and ∼0.07 mag respectively. The extinction maps successfully separate the clouds that overlap in the sky area and manifest the structure of the individual cloud. Meanwhile, a bow-like structure is found with a distance range from 175 to 250 pc, half of which is a part of the Per-Tau Shell in similar coordinates and distance while the other half is not. Three low-extinction rings are additionally discovered and briefly discussed.
Constraining a Model of the Radio Sky below 6 MHz Using the Parker Solar Probe/FIELDS Instrument in Preparation for Upcoming Lunar-based Experiments
Authors: Bassett Neil , Rapetti David , Nhan Bang D. , Page Brent , Burns Jack O. , Pulupa Marc , Bale Stuart D. 
Published: March 2023

Abstract
We present a Bayesian analysis of data from the FIELDS instrument on board the Parker Solar Probe (PSP) spacecraft with the aim of constraining low-frequency (≲6 MHz) sky in preparation for several upcoming lunar-based experiments. We utilize data recorded during PSP’s coning roll maneuvers, in which the axis of the spacecraft is pointed 45° off of the Sun. The spacecraft then rotates about a line between the Sun and the spacecraft with a period of 24 minutes. We reduce the data into two formats: roll-averaged, in which the spectra are averaged over the roll, and phase-binned, in which the spectra are binned according to the phase of the roll. We construct a forward model of the FIELDS observations that includes numerical simulations of the antenna beam, an analytic emissivity function of the galaxy, and estimates of the absorption due to free electrons. Fitting 5 parameters, we find that the roll-averaged data can be fit well by this model, and we obtain posterior parameter constraints that are in general agreement with previous estimates. The model is not, however, able to fit the phase-binned data well, likely due to limitations such as the lack of nonsmooth emission structure at both small and large scales, enforced symmetry between the northern and southern galactic hemispheres, and large uncertainties in the free electron density. This suggests that significant improvement in the low-frequency sky model is needed in order to fully and accurately represent the sky at frequencies below 6 MHz.
Observational Evidence for Large-scale Gas Heating in a Galaxy Protocluster at z = 2.30
Authors: Dong Chenze , Lee Khee-Gan , Ata Metin , Horowitz Benjamin , Momose Rieko 
Published: March 2023

Abstract
We report a z = 2.30 galaxy protocluster (COSTCO-I) in the COSMOS field, where the Lyα forest as seen in the CLAMATO IGM tomography survey does not show significant absorption. This departs from the transmission–density relationship (often dubbed the fluctuating Gunn–Peterson approximation; FGPA) usually expected to hold at this epoch, which would lead one to predict strong Lyα absorption at the overdensity. For comparison, we generate mock Lyα forest maps by applying the FGPA to constrained simulations of the COSMOS density field and create mocks that incorporate the effects of finite sight-line sampling, pixel noise, and Wiener filtering. Averaged over r = 15 h
−1 Mpc around the protocluster, the observed Lyα forest is consistently more transparent in the real data than in the mocks, indicating a rejection of the null hypothesis that the gas in COSTCO-I follows the FGPA (p = 0.0026, or 2.79σ significance). It suggests that the large-scale gas associated with COSTCO-I is being heated above the expectations of the FGPA, which might be due to either large-scale AGN jet feedback or early gravitational shock heating. COSTCO-I is the first known large-scale region of the IGM that is observed to be transitioning from the optically thin photoionized regime at cosmic noon to eventually coalesce into an intracluster medium (ICM) by z = 0. Future observations of similar structures will shed light on the growth of the ICM and allow constraints on AGN feedback mechanisms.