bluuebunny/crossref_metadata_2025 huggingface dataset:
Frontal dermoid cyst coexisting with suprasellar craniopharyngioma: a spectrum of ectodermally derived epithelial-lined cystic lesions?
Authors: Abou-Al-Shaar Hussam , Abd-El-Barr Muhammad M. , Zaidi Hasan A. , Russell-Goldman Eleanor , Folkerth Rebecca D. , Laws Edward R. , Chiocca E. Antonio
Published: December 2016

There is a wide group of lesions that may exist in the sellar and suprasellar regions. Embryologically, there is varying evidence that many of these entities may in fact represent a continuum of pathology deriving from a common ectodermal origin. The authors report a case of a concomitant suprasellar craniopharyngioma invading the third ventricle with a concurrent frontal lobe cystic dermoid tumor. A 21-year-old man presented to the authors' service with a 3-day history of worsening headache, nausea, vomiting, and blurry vision. Magnetic resonance imaging depicted a right frontal lobe lesion associated with a separate suprasellar cystic lesion invading the third ventricle. The patient underwent a right pterional craniotomy for resection of both lesions. Gross-total resection of the right frontal lesion was achieved, and subtotal resection of the suprasellar lesion was accomplished with some residual tumor adherent to the walls of the third ventricle. Histopathological examination of the resected right frontal lesion documented a diagnosis of dermoid cyst and, for the suprasellar lesion, a diagnosis of adamantinomatous craniopharyngioma. The occurrence of craniopharyngioma with dermoid cyst has not been reported in the literature before. Such an association might indeed suggest the previously reported hypothesis that these lesions represent a spectrum of ectodermally derived epithelial-lined cystic lesions.
Molecular pathology of adamantinomatous craniopharyngioma: review and opportunities for practice
Authors: Apps John Richard , Martinez-Barbera Juan Pedro
Published: December 2016

Since the first identification of CTNNB1 mutations in adamantinomatous craniopharyngioma (ACP), much has been learned about the molecular pathways and processes that are disrupted in ACP pathogenesis. To date this understanding has not translated into tangible patient benefit.

The recent development of novel techniques and a range of preclinical models now provides an opportunity to begin to support treatment decisions and develop new therapeutics based on molecular pathology.

In this review the authors summarize many of the key findings and pathways implicated in ACP pathogenesis and discuss the challenges that need to be tackled to translate these basic science findings for the benefit of patients.
Microscopic versus endoscopic approaches for craniopharyngiomas: choosing the optimal surgical corridor for maximizing extent of resection and complication avoidance using a personalized, tailored approach
Authors: Liu James K. , Sevak Ilesha A. , Carmel Peter W. , Eloy Jean Anderson
Published: December 2016

Resection remains the mainstay of treatment for craniopharyngiomas with the goal of radical resection, if safely possible, to minimize the rate of recurrence. Endoscopic endonasal and microscopic transcranial surgical approaches have both become standard methods for the treatment for craniopharyngiomas. However, the approach selection paradigm for craniopharyngiomas is still a point of discussion. Choosing the optimal surgical approach can play a significant role in maximizing the extent of resection and surgical outcome while minimizing the risks of potential complications. Craniopharyngiomas can present with a variety of different sizes, locations, and tumor consistencies, and each individual tumor has distinct features that favor one specific approach over another. The authors review standard cranial base techniques applied to craniopharyngioma surgery, using both the endoscopic endonasal approach and traditional open microsurgical approaches, and analyze factors involved in approach selection. They discuss their philosophy of approach selection based on the location and extent of the tumor on preoperative imaging as well as the advantages and limitations of each surgical corridor, and they describe the operative nuances of each technique, using a personalized, tailored approach to the individual patient with illustrative cases and videos.
Endoscopic endonasal versus open transcranial resection of craniopharyngiomas: a case-matched single-institution analysis
Authors: Moussazadeh Nelson , Prabhu Vishaal , Bander Evan D. , Cusic Ryan C. , Tsiouris Apostolos John , Anand Vijay K. , Schwartz Theodore H.
Published: December 2016

OBJECTIVE

The authors compared clinical and radiological outcomes after resection of midline craniopharyngiomas via an endoscopic endonasal approach (EEA) versus an open transcranial approach (TCA) at a single institution in a series in which the tumors were selected to be equally amenable to gross-total resection (GTR) with either approach.

METHODS

A single-institution retrospective review of previously untreated adult midline craniopharyngiomas was performed. Lesions were evaluated by 4 neurosurgeons blinded to the actual approach used to identify cases that were equally amenable to GTR using either an EEA or TCA. Radiological and clinical outcome data were assessed.

RESULTS

Twenty-six cases amenable to either approach were identified, 21 EEA and 5 TCA. Cases involving tumors that were resected via a TCA had a trend toward larger diameter (p = 0.10) but were otherwise equivalent in preoperative clinical and radiological characteristics. GTR was achieved in a greater proportion of cases removed with an EEA than a TCA (90% vs 40%, respectively; p = 0.009). Endoscopic resection was associated with superior visual restoration (63% vs 0%; p < 0.05), a decreased incidence of recurrence (p < 0.001), lower increase in FLAIR signal postoperatively (−0.16 ± 4.6 cm3 vs 14.4 ± 14.0 cm3; p < 0.001), and fewer complications (20% vs 80% of patients; p < 0.001). Significantly more TCA patients suffered postoperative cognitive loss (80% vs 0; p < 0.0001).

CONCLUSIONS

An EEA is a safe and effective approach to suprasellar craniopharyngiomas amenable to GTR. For this select group of cases, the EEA may provide higher rates of GTR and visual improvement with fewer complications compared with a TCA.
Drug priming enhances radiosensitivity of adamantinomatous craniopharyngioma via downregulation of survivin
Authors: Stache Christina , Bils Christiane , Fahlbusch Rudolf , Flitsch Jörg , Buchfelder Michael , Stefanits Harald , Czech Thomas , Gaipl Udo , Frey Benjamin , Buslei Rolf , Hölsken Annett
Published: December 2016

OBJECTIVE

In this study, the authors investigated the underlying mechanisms responsible for high tumor recurrence rates of adamantinomatous craniopharyngioma (ACP) after radiotherapy and developed new targeted treatment protocols to minimize recurrence. ACPs are characterized by the activation of the receptor tyrosine kinase epidermal growth factor receptor (EGFR), known to mediate radioresistance in various tumor entities. The impact of tyrosine kinase inhibitors (TKIs) gefitinib or CUDC-101 on radiation-induced cell death and associated regulation of survivin gene expression was evaluated.

METHODS

The hypothesis that activated EGFR promotes radioresistance in ACP was investigated in vitro using human primary cell cultures of ACP (n = 10). The effects of radiation (12 Gy) and combined radiochemotherapy on radiosensitivity were assessed via cell death analysis using flow cytometry. Changes in target gene expression were analyzed by quantitative real-time polymerase chain reaction (qRT-PCR). Survivin, identified in qRT-PCR to be involved in radioresistance of ACP, was manipulated by small interfering RNA (siRNA), followed by proliferation and vitality assays to further clarify its role in ACP biology. Immunohistochemically, survivin expression was assessed in patient tumors used for primary cell cultures.

RESULTS

In primary human ACP cultures, activation of EGFR resulted in significantly reduced cell death levels after radiotherapy. Treatment with TKIs alone and in combination with radiotherapy increased cell death response remarkably, assessed by flow cytometry. CUDC-101 was significantly more effective than gefitinib. The authors identified regulation of survivin expression after therapeutic intervention as the underlying molecular mechanism of radioresistance in ACP. EGFR activation promoting ACP cell survival and proliferation in vitro is consistent with enhanced survivin gene expression shown by qRT-PCR. TKI treatment, as well as the combination with radiotherapy, reduced survivin levels in vitro. Accordingly, ACP showed reduced cell viability and proliferation after survivin downregulation by siRNA.

CONCLUSIONS

These results indicate an impact of EGFR signaling on radioresistance in ACP. Inhibition of EGFR activity by means of TKI treatment acts as a radiosensitizer on ACP tumor cells, leading to increased cell death. Additionally, the results emphasize the antiapoptotic and pro-proliferative role of survivin in ACP biology and its regulation by EGFR signaling. The suppression of survivin by treatment with TKI and combined radiotherapy represents a new promising treatment strategy that will be further assessed in in vivo models of ACP.
Postoperative outcome of body core temperature rhythm and sleep-wake cycle in third ventricle craniopharyngiomas
Authors: Zoli Matteo , Sambati Luisa , Milanese Laura , Foschi Matteo , Faustini-Fustini Marco , Marucci Gianluca , de Biase Dario , Tallini Giovanni , Cecere Annagrazia , Mignani Francesco , Sturiale Carmelo , Frank Giorgio , Pasquini Ernesto , Cortelli Pietro , Mazzatenta Diego , Provini Federica
Published: December 2016

OBJECTIVE

One of the more serious risks in the treatment of third ventricle craniopharyngiomas is represented by hypothalamic damage. Recently, many papers have reported the expansion of the indications for the endoscopic endonasal approach (EEA) to be used for these tumors as well. The aim of this study was to assess the outcome of sleep-wake cycle and body core temperature (BCT), both depending on hypothalamic control, in patients affected by craniopharyngiomas involving the third ventricle that were surgically treated via an EEA.

METHODS

All consecutive adult patients with craniopharyngiomas that were treated at one center via an EEA between 2014 and 2016 were prospectively included. Each patient underwent neuroradiological, endocrinological, and ophthalmological evaluation; 24-hour monitoring of the BCT rhythm; and the sleep-wake cycle before surgery and at follow-up of at least 6 months.

RESULTS

Ten patients were included in the study (male/female ratio 4:6, mean age 48.6 years, SD 15.9 years). Gross-total resection was achieved in 8 cases. Preoperative BCT rhythm was pathological in 6 patients. After surgery, these disturbances resolved in 2 cases, improved in another 3, and remained the same in 1 patient; also, 1 case of de novo onset was observed. Before surgery the sleep-wake cycle was pathological in 8 cases, and it was restored in 4 patients at follow-up. After surgery the number of patients reporting diurnal naps increased from 7 to 9.

CONCLUSIONS

The outcome of the sleep-wake cycle and BCT analyzed after EEA in this study is promising. Despite the short duration of the authors' experience, they consider these results encouraging; additional series are needed to confirm the preliminary findings.
Diagnosis and management of craniopharyngiomas in the era of genomics and targeted therapy
Authors: Martinez-Gutierrez Juan Carlos , D'Andrea Megan R. , Cahill Daniel P. , Santagata Sandro , Barker Fred G. , Brastianos Priscilla K.
Published: December 2016

Craniopharyngiomas are rare intracranial neoplasms that pose clinical challenges due to their location adjacent to vital structures. The authors have previously shown high mutation rates of BRAF V600E in papillary craniopharyngioma and of CTNNB1 in adamantinomatous craniopharyngioma. These activating driver mutations are potential therapeutic targets, and the authors have recently reported a significant response to BRAF/MEK inhibition in a patient with multiply recurrent PCP. As these targetable mutations warrant prospective research, the authors will be conducting a national National Cancer Institute–sponsored multicenter clinical trial to investigate BRAF/MEK inhibition in the treatment of craniopharyngioma. In this new era of genomic discovery, the treatment paradigm of craniopharyngioma is likely to change.
Gagea saxatilis (Mert. et Koch) Schultes et Schultes (Liliacées), nouvelles stations ardéchoises
Authors: Delaigue Jacques
Published: December 2016

Mise au point sur la distribution et l'écologie de G. saxatilis dans la vallée du Rhône et présentation de deux nouvelles stations en Ardèche.
Sur l'usage des notions d'ovule et de graine en Botanique et en Paéobotanique
Authors: Lemoigne Yves
Published: December 2016

Les paléobotanistes désignent indifféremment sous l'appellation «graine» (seed, des auteurs de langue anglaise) les éléments de dispersion des Spermatophytes et des Préspermatophytes, dans le cadre de la reproduction sexuée. Or, il importe de bien distinguer, d'une part, la «graine » propre aux Spermato¬ phytes, d'autre part, l'«ovule » qui est l'élément dispersé par les Préspermatophytes. La distinction entre ovule et graine est tout à fait comparable à celle que nous faisons entre spore et grain de pollen. Cette distinction est d'autant plus nécessaire que nous avons déjà proposé la substitution de l'appellation Préspermatophytes à celle de Préphanérogames dans la mesure où, précisément, il s'agit d'un taxon regroupant des plantes «annonçant » la graine.
THE [Ne iii] JET OF DG Tau AND ITS IONIZATION SCENARIOS
Authors: Liu Chun-Fan , Shang Hsien , Herczeg Gregory J. , Walter Frederick M.
Published: December 2016

Forbidden neon emission from jets of low-mass young stars can be used to probe the underlying high-energy processes in these systems. We analyze spectra of the jet of DG Tau obtained with the Very Large Telescope/X-Shooter spectrograph in 2010. [Ne iii]

is clearly detected in the innermost 3″ microjet and the outer knot located at

. The velocity structure of the inner microjet can be decomposed into the low-velocity component at

km s−1 and the high-velocity component (HVC) at

km s−1. Based on the observed [Ne iii] flux and its spatial extent, we suggest the origins of the [Ne iii] emission regions and their relation with known X-ray sources along the jet. The flares from the hard X-ray source close to the star may be the main ionization source of the innermost microjet. The fainter soft X-ray source at

from the star may provide sufficient heating to help to sustain the ionization fraction against recombination in the flow. The outer knot may be reionized by shocks faster than 100 km s−1 such that [Ne iii] emission reappears and the soft X-ray emission at

is produced. Velocity decomposition of the archival Hubble Space Telescope spectra obtained in 1999 shows that the HVC had been faster, with a velocity centroid of

km s−1. Such a decrease in velocity may potentially be explained by the expansion of the stellar magnetosphere, changing the truncation radius and thus the launching speed of the jet. The energy released by magnetic reconnections during relaxation of the transition can heat the gas up to several tens of megakelvin and provide the explanation for on-source keV X-ray flares that ionize the neon microjet.
ON THE ROTATION SPEED OF THE MILKY WAY DETERMINED FROM H i EMISSION
Authors: Reid M. J. , Dame T. M.
Published: December 2016

The circular rotation speed of the Milky Way at the solar radius, Θ0, has been estimated to be 220 km s−1 by fitting the maximum velocity of H i emission as a function of Galactic longitude. This result is in tension with a recent estimate of Θ0 = 240 km s−1, based on Very Long Baseline Interferometry (VLBI) parallaxes and proper motions from the BeSSeL and VERA surveys for large numbers of high-mass star-forming regions across the Milky Way. We find that the rotation curve best fitted to the VLBI data is slightly curved, and that this curvature results in a biased estimate of Θ0 from the H i data when a flat rotation curve is assumed. This relieves the tension between the methods and favors Θ0 = 240 km s−1.
VLT FORS2 COMPARATIVE TRANSMISSION SPECTROSCOPY: DETECTION OF Na IN THE ATMOSPHERE OF WASP-39b FROM THE GROUND
Authors: Nikolov Nikolay , Sing David K. , Gibson Neale P. , Fortney Jonathan J. , Evans Thomas M. , Barstow Joanna K. , Kataria Tiffany , Wilson Paul A.
Published: December 2016

We present transmission spectroscopy of the warm Saturn-mass exoplanet WASP-39b made with the Very Large Telescope FOcal Reducer and Spectrograph (FORS2) across the wavelength range 411–810 nm. The transit depth is measured with a typical precision of 240 parts per million (ppm) in wavelength bins of 10 nm on a V = 12.1 mag star. We detect the sodium absorption feature (3.2σ) and find evidence of potassium. The ground-based transmission spectrum is consistent with Hubble Space Telescope (HST) optical spectroscopy, supporting the interpretation that WASP-39b has a largely clear atmosphere. Our results demonstrate the great potential of the recently upgraded FORS2 spectrograph for optical transmission spectroscopy, with which we obtained HST-quality light curves from the ground.
DEPENDENCE OF SMALL PLANET FREQUENCY ON STELLAR METALLICITY HIDDEN BY THEIR PREVALENCE
Authors: Zhu 祝伟 Wei , Wang 王吉 Ji , Huang 黄煦 Chelsea
Published: December 2016

The dependence of gas giant planet occurrence rate on stellar metallicity has been firmly established. We extend this so-called planet–metallicity correlation to broader ranges of metallicities and planet masses/radii. In particular, we assume that the planet–metallicity correlation is a power law below some critical saturation threshold, and that the probability of hosting at least one planet is unity for stars with metallicity above the threshold. We then are able to explain the discrepancy between the tentative detection and null detection in previous studies regarding the planet–metallicity correlation for small planets. In particular, we find that the null detection of this correlation can be attributed to the combination of high planet occurrence rate and low detection efficiency. Therefore, a planet–metallicity correlation for small planets cannot be ruled out. We propose that stars with metallicities lower than the solar value are better targets for testing the planet–metallicity correlation for small planets.
IMPROVING THE FLUX CALIBRATION IN REVERBERATION MAPPING BY SPECTRAL FITTING:APPLICATION TO THE SEYFERT GALAXY MCG–6-30-15
Authors: Hu Chen , Wang Jian-Min , Ho Luis C. , Bai Jin-Ming , Li Yan-Rong , Du Pu , Lu Kai-Xing
Published: December 2016

We propose a method for the flux calibration of reverberation mapping spectra, based on accurate measurement of [O iii] λ5007 emission by spectral fitting. Our method can achieve better accuracy than the traditional method of Groningen & Wanders, allowing reverberation mapping measurements for objects with variability amplitudes as low as ∼5%. As a demonstration, we reanalyze the data of the Seyfert 1 galaxy MCG–6-30-15, taken from the 2008 campaign of the Lick active galactic nucleus monitoring project, which previously failed to obtain a time lag for this weakly variable object, owing to a relatively large flux calibration uncertainty. We detect a statistically significant rest-frame time lag of

days between the Hβ and V-band light curves. Combining this lag with FWHM(Hβ) = 1933 ± 81 km s−1 and a virial coefficient of f = 0.7, we derive a virial black hole mass of

M
⊙, which agrees well with previous estimates by other methods.
STACKING SPECTRA IN PROTOPLANETARY DISKS: DETECTING INTENSITY PROFILES FROM HIDDEN MOLECULAR LINES IN HD 163296
Authors: Yen Hsi-Wei , Koch Patrick M. , Liu Hauyu Baobab , Puspitaningrum Evaria , Hirano Naomi , Lee Chin-Fei , Takakuwa Shigehisa
Published: December 2016

We introduce a new stacking method in Keplerian disks that (1) enhances signal-to-noise ratios (S/Ns) of detected molecular lines and (2) makes visible otherwise-undetectable weak lines. Our technique takes advantage of the Keplerian rotational velocity pattern. It aligns spectra according to their different centroid velocities at their different positions in a disk and stacks them. After aligning, the signals are accumulated in a narrower velocity range as compared to the original line width without alignment. Moreover, originally correlated noise becomes decorrelated. Stacked and aligned spectra thus have a higher S/N. We apply our method to Atacama Large Millimeter/Submillimeter Array (ALMA) archival data of DCN (3–2), DCO+ (3–2), N2D+ (3–2), and H2CO (3

–2

), (3

–2

), and (3

–2

) in the protoplanetary disk around HD 163296. As a result, (1) the S/Ns of the originally detected DCN (3–2), DCO+ (3–2), H2CO (3

–2

), and N2D+ (3–2) lines are boosted by a factor of ≳4–5 at their spectral peaks, implying one order of magnitude shorter integration times to reach the original S/N; and (2) the previously undetectable spectra of the H2CO (3

–2

) and (3

–2

) lines are materialized at more than 3σ. These dramatically enhanced S/Ns allow us to measure intensity distributions in all lines with high significance. The principle of our method can be applied not only to Keplerian disks but also to any systems with ordered kinematic patterns.
DISCOVERY OF INFALLING MOTION WITH ROTATION OF THE CLUSTER-FORMING CLUMP S235AB AND ITS IMPLICATION TO THE CLUMP STRUCTURES
Authors: Shimoikura Tomomi , Dobashi Kazuhito , Matsumoto Tomoaki , Nakamura Fumitaka
Published: December 2016

We report the discovery of infalling motion with the rotation of S235AB, a massive cluster-forming clump (

) in the S235 region. Our C18O observations with the 45 m telescope at the Nobeyama Radio Observatory have revealed an elliptical shape of the clump. A position–velocity diagram taken along its major axis exhibits two well-defined peaks symmetrically located, with respect to the clump center. This is similar to that found for a dynamically infalling envelope with rotation around a single protostar, modeled by N. Ohashi et al., indicating that the cluster-forming clump is also collapsing by the self-gravity toward the clump center. With analogue to Ohashi et al.'s model, we made a simple model of an infalling, rotating clump to fit the observed data. Based on the inferred model parameters, as well as results of earlier observations and simulations in the literature, we discuss the structures of the clump such as the relation among the global mass infall rate (

yr−1), formation of a compact core (with a mass and size of ∼4

and

pc) at the center, and a massive star (∼11

) forming in the core.
THE STELLAR DENSITY PROFILE OF THE DISTANT GALACTIC HALO
Authors: Slater Colin T. , Nidever David L. , Munn Jeffrey A. , Bell Eric F. , Majewski Steven R.
Published: December 2016

We use extensive gravity-sensitive DDO 51 photometry over 5100 square degrees, combined with Sloan Digital Sky Survey broadband photometry, to select a catalog of ∼4000 giant stars covering a large fraction of the high Galactic latitude sky and reaching out to ∼80 kpc in the Galactic halo. This sample of bright and unbiased tracers enables us to measure the radial profile and 3D structure of the stellar halo to large distances, which had previously only been measured with sparse tracers or small samples. Using population synthesis models to reproduce the observed giant star luminosity function, we find that the halo maintains a

r

−
3.5

profile from 30 to 80 kpc with no signs of a truncation or sharp break over this range. The radial profile measurement is largely insensitive to individual halo substructure components, but we find that attempting to measure the shape of the halo is overwhelmed by the Sagittarius stream such that no elliposidal shape is a satisfactory description in this region. These measurements allow us to begin placing the Milky Way in context with the growing sample of external galaxies where similar halo profile measurements are available, with the goal of further linking the properties of stellar halos to the accretion histories that formed them.
THE CARNEGIE-CHICAGO HUBBLE PROGRAM. I. AN INDEPENDENT APPROACH TO THE EXTRAGALACTIC DISTANCE SCALE USING ONLY POPULATION II DISTANCE INDICATORS*
Authors: Beaton Rachael L. , Freedman Wendy L. , Madore Barry F. , Bono Giuseppe , Carlson Erika K. , Clementini Gisella , Durbin Meredith J. , Garofalo Alessia , Hatt Dylan , Jang In Sung , Kollmeier Juna A. , Lee Myung Gyoon , Monson Andrew J. , Rich Jeffrey A. , Scowcroft Victoria , Seibert Mark , Sturch Laura , Yang Soung-Chul
Published: December 2016

We present an overview of the Carnegie-Chicago Hubble Program, an ongoing program to obtain a 3% measurement of the Hubble constant (H
0) using alternative methods to the traditional Cepheid distance scale. We aim to establish a completely independent route to H
0 using RR Lyrae variables, the tip of the red giant branch (TRGB), and Type Ia supernovae (SNe Ia). This alternative distance ladder can be applied to galaxies of any Hubble type, of any inclination, and, using old stars in low-density environments, is robust to the degenerate effects of metallicity and interstellar extinction. Given the relatively small number of SNe Ia host galaxies with independently measured distances, these properties provide a great systematic advantage in the measurement of H
0 via the distance ladder. Initially, the accuracy of our value of H
0 will be set by the five Galactic RR Lyrae calibrators with Hubble Space Telescope Fine-Guidance Sensor parallaxes. With Gaia, both the RR Lyrae zero-point and TRGB method will be independently calibrated, the former with at least an order of magnitude more calibrators and the latter directly through parallax measurement of tip red giants. As the first end-to-end “distance ladder” completely independent of both Cepheid variables and the Large Magellanic Cloud, this path to H
0 will allow for the high-precision comparison at each rung of the traditional distance ladder that is necessary to understand tensions between this and other routes to H
0.
WIDE-BAND SPECTRA OF GIANT RADIO PULSES FROM THE CRAB PULSAR
Authors: Mikami Ryo , Asano Katsuaki , Tanaka Shuta J. , Kisaka Shota , Sekido Mamoru , Takefuji Kazuhiro , Takeuchi Hiroshi , Misawa Hiroaki , Tsuchiya Fuminori , Kita Hajime , Yonekura Yoshinori , Terasawa Toshio
Published: December 2016

We present the results of the simultaneous observation of giant radio pulses (GRPs) from the Crab pulsar at 0.3, 1.6, 2.2, 6.7, and 8.4 GHz with four telescopes in Japan. We obtain 3194 and 272 GRPs occurring at the main pulse and the interpulse phases, respectively. A few GRPs detected at both 0.3 and 8.4 GHz are the most wide-band samples ever reported. In the frequency range from 0.3 to 2.2 GHz, we find that about 70% or more of the GRP spectra are consistent with single power laws and their spectral indices are distributed from −4 to −1. We also find that a significant number of GRPs have such a hard spectral index (approximately −1) that the fluence at 0.3 GHz is below the detection limit (“dim-hard” GRPs). Stacking light curves of such dim-hard GRPs at 0.3 GHz, we detect consistent enhancement compared to the off-GRP light curve. Our samples show apparent correlations between the fluences and the spectral hardness, which indicates that more energetic GRPs tend to show softer spectra. Our comprehensive studies on the GRP spectra are useful materials to verify the GRP model of fast radio bursts in future observations.
THE 6 μm FEATURE AS A TRACER OF ALIPHATIC COMPONENTS OF INTERSTELLAR CARBONACEOUS GRAINS
Authors: Hsia 夏志浩 Chih-Hao , Sadjadi Seyedabdolreza , Zhang 張泳 Yong , Kwok 郭新 Sun
Published: December 2016

An unidentified infrared emission (UIE) feature at 6.0 μm is detected in a number of astronomical sources showing the UIE bands. In contrast to the previous suggestion that this band is due to C=O vibrational modes, we suggest that the 6.0 μm feature arises from olefinic double-bond functional groups. These groups are likely to be attached to aromatic rings, which are responsible for the major UIE bands. The possibility that the formation of these functional groups is related to the hydrogenation process is discussed.
VLA AND ALMA IMAGING OF INTENSE GALAXY-WIDE STAR FORMATION IN z ∼ 2 GALAXIES
Authors: Rujopakarn W. , Dunlop J. S. , Rieke G. H. , Ivison R. J. , Cibinel A. , Nyland K. , Jagannathan P. , Silverman J. D. , Alexander D. M. , Biggs A. D. , Bhatnagar S. , Ballantyne D. R. , Dickinson M. , Elbaz D. , Geach J. E. , Hayward C. C. , Kirkpatrick A. , McLure R. J. , Michałowski M. J. , Miller N. A. , Narayanan D. , Owen F. N. , Pannella M. , Papovich C. , Pope A. , Rau U. , Robertson B. E. , Scott D. , Swinbank A. M. , Werf P. van der , Kampen E. van , Weiner B. J. , Windhorst R. A.
Published: December 2016

We present ≃0.″4 resolution extinction-independent distributions of star formation and dust in 11 star-forming galaxies (SFGs) at z = 1.3–3.0. These galaxies are selected from sensitive blank-field surveys of the 2′ × 2′ Hubble Ultra-Deep Field at λ = 5 cm and 1.3 mm using the Karl G. Jansky Very Large Array and Atacama Large Millimeter/submillimeter Array. They have star formation rates (SFRs), stellar masses, and dust properties representative of massive main-sequence SFGs at z ∼ 2. Morphological classification performed on spatially resolved stellar mass maps indicates a mixture of disk and morphologically disturbed systems; half of the sample harbor X-ray active galactic nuclei (AGNs), thereby representing a diversity of z ∼ 2 SFGs undergoing vigorous mass assembly. We find that their intense star formation most frequently occurs at the location of stellar-mass concentration and extends over an area comparable to their stellar-mass distribution, with a median diameter of 4.2 ± 1.8 kpc. This provides direct evidence of galaxy-wide star formation in distant blank-field-selected main-sequence SFGs. The typical galactic-average SFR surface density is 2.5 M
⊙ yr−1 kpc−2, sufficiently high to drive outflows. In X-ray-selected AGN where radio emission is enhanced over the level associated with star formation, the radio excess pinpoints the AGNs, which are found to be cospatial with star formation. The median extinction-independent size of main-sequence SFGs is two times larger than those of bright submillimeter galaxies, whose SFRs are 3–8 times larger, providing a constraint on the characteristic SFR (∼300 M
⊙ yr−1) above which a significant population of more compact SFGs appears to emerge.
INTERACTION BETWEEN THE SUPERNOVA REMNANT HB 3 AND THE NEARBY STAR-FORMING REGION W3
Authors: Zhou Xin , Yang Ji , Fang Min , Su Yang , Sun Yan , Chen Yang
Published: December 2016

We performed millimeter observations of CO lines toward the supernova remnant (SNR) HB 3. Substantial molecular gas around −45 km s−1 is detected in the conjunction region between the SNR HB 3 and the nearby W3 complex. This molecular gas is distributed along the radio continuum shell of the remnant. Furthermore, the shocked molecular gas indicated by line wing broadening features is also distributed along the radio shell and inside it. By both morphological correspondence and dynamical evidence, we confirm that the SNR HB 3 interacts with the −45 km s−1 molecular cloud (MC), in essence, with the nearby H ii region/MC complex W3. The redshifted line wing broadening features indicate that the remnant is located at the nearside of the MC. With this association, we could place the remnant at the same distance as the W3/W4 complex, which is 1.95 ± 0.04 kpc. The spatial distribution of aggregated young stellar object candidates shows a correlation with the shocked molecular strip associated with the remnant. We also find a binary clump of CO at (l = 132.°94, b = 1.°12) around −51.5 km s−1 inside the projected extent of the remnant, and it is associated with significant mid-infrared emission. The binary system also has a tail structure resembling the tidal tails of interacting galaxies. According to the analysis of CO emission lines, the larger clump in this binary system is about stable, and the smaller clump is significantly disturbed.
GLOBAL INSTABILITY OF THE EXO-MOON SYSTEM TRIGGERED BY PHOTO-EVAPORATION
Authors: Yang Ming , Xie Ji-Wei , Zhou Ji-Lin , Liu Hui-Gen , Zhang Hui
Published: December 2016

Many exoplanets have been found in orbits close to their host stars and thus they are subject to the effects of photo-evaporation. Previous studies have shown that a large portion of exoplanets detected by the Kepler mission have been significantly eroded by photo-evaporation. In this paper, we numerically study the effects of photo-evaporation on the orbital evolution of a hypothesized moon system around a planet. We find that photo-evaporation is crucial to the stability of the moon system. Photo-evaporation can erode the atmosphere of the planet thus leading to significant mass loss. As the planet loses mass, its Hill radius shrinks and its moons increase their orbital semimajor axes and eccentricities. When some moons approach their critical semimajor axes, global instability of the moon system would be triggered, which usually ends up with two, one or even zero surviving moons. Some lost moons could escape from the moon system to become a new planet orbiting the star or run away further to become a free-floating object in the Galaxy. Given the destructive role of photo-evaporation, we speculate that exomoons are less common for close-in planets (<0.1 au), especially those around M-type stars, because they are more X-ray luminous and thus enhancing photo-evaporation. The lessons we learn in this study may be helpful for the target selection of on-going/future exomoon searching programs.
EVOLUTION OF THE MASS AND LUMINOSITY FUNCTIONS OF GLOBULAR STAR CLUSTERS
Authors: Goudfrooij Paul , Fall S. Michael
Published: December 2016

We reexamine the dynamical evolution of the mass and luminosity functions of globular star clusters (GCMF and GCLF). Fall & Zhang (2001, FZ01) showed that a power-law MF, as commonly seen among young cluster systems, would evolve by dynamical processes over a Hubble time into a peaked MF with a shape very similar to the observed GCMF in the Milky Way and other galaxies. To simplify the calculations, the semi-analytical FZ01 model adopted the “classical” theory of stellar escape from clusters, and neglected variations in the

/L ratios of clusters. Kruijssen & Portegies Zwart (2009, KPZ09) modified the FZ01 model to include “retarded” and mass-dependent stellar escape, the latter causing significant

/L variations. KPZ09 asserted that their model was compatible with observations, whereas the FZ01 model was not. We show here that this claim is not correct; the FZ01 and KPZ09 models fit the observed Galactic GCLF equally well. We also show that there is no detectable correlation between

/L and L for GCs in the Milky Way and Andromeda galaxies, in contradiction with the KPZ09 model. Our comparisons of the FZ01 and KPZ09 models with observations can be explained most simply if stars escape at rates approaching the classical limit for high-mass clusters, as expected on theoretical grounds.
VENUS CLOUD MORPHOLOGY AND MOTIONS FROM GROUND-BASED IMAGES AT THE TIME OF THE AKATSUKI ORBIT INSERTION∗
Authors: Sánchez-Lavega A. , Peralta J. , Gomez-Forrellad J. M. , Hueso R. , Pérez-Hoyos S. , Mendikoa I. , Rojas J. F. , Horinouchi T. , Lee Y. J. , Watanabe S.
Published: December 2016

We report Venus image observations around the two maximum elongations of the planet at 2015 June and October. From these images we describe the global atmospheric dynamics and cloud morphology in the planet before the arrival of JAXA’s Akatsuki mission on 2015 December 7. The majority of the images were acquired at ultraviolet wavelengths (380–410 nm) using small telescopes. The Venus dayside was also observed with narrowband filters at other wavelengths (890 nm, 725–950 nm, 1.435 μm CO2 band) using the instrument PlanetCam-UPV/EHU at the 2.2 m telescope in Calar Alto Observatory. In all cases, the lucky imaging methodology was used to improve the spatial resolution of the images over the atmospheric seeing. During the April–June period, the morphology of the upper cloud showed an irregular and chaotic texture with a well-developed equatorial dark belt (afternoon hemisphere), whereas during October–December the dynamical regime was dominated by planetary-scale waves (Y-horizontal, C-reversed, and ψ-horizontal features) formed by long streaks, and banding suggesting more stable conditions. Measurements of the zonal wind velocity with cloud tracking in the latitude range from 50°N to 50°S shows agreement with retrievals from previous works.
The Family and Mortality: A Case Study from Rural Belgium
Authors: Alter George , Oris Michel , Broström Göran
Published: December 2016

Résumé Les différences de mortalité entre les familles fournissent un indice de l'importance des comportements inobservés conditionnant à la santé. Par exemple, si la plus faible mortalité était due à des attitudes personnelles apprises au cours de l'enfance, elle devrait se manifester jusqu'aux âges élevés. Dans cet article sont utilisées des données provenant d'une commune belge, au xix e siècle, afin de préciser les différences de mortalité entre les familles de deux manières. Tout d'abord, un indice de l'exposition des enfants à la maladie est construit en comptant le nombre de décès à moins de 15 ans dans chaque famille. Ensuite, l'effet global des différences entre les familles est calculé grâce à un modèle aléatoire qui permet d'estimer la variance de « l'effet famille ». Les deux mesures mettent en évidence un effet familial fort pendant l'enfance, qui diminue après 15 ans puis disparaît au-delà de 55 ans. En outre, à une période encore dominée par les maladies infectieuses, ceux qui survivent aux maladies contractées au cours de l'enfance acquièrent des immunités qui les rendent plus résistants par la suite.
La gangrène gazeuse pendant la Première Guerre mondiale (Front occidental)
Authors: Debue-Barazer Christine
Published: December 2016

Résumé Maladie infectieuse aiguë des parties molles, la gangrène gazeuse apparaît comme la complication la plus grave des plaies de guerre dès les premières offensives de l'automne 1914. Les médecins, surpris et impuissants, croient à l'émergence d'une nouvelle maladie. Or, au fil des mois on comprend que dans cette guerre de position tout concourt à favoriser le développement d'un mal connu depuis l'Antiquité : les blessures par éclats d'obus, l'immobilisation des soldats dans des tranchées insalubres, la pauvreté et la médiocrité des équipements sanitaires, l'acheminement lent et mal conduit des blessés vers l'arrière, les soins mal adaptés. Les équipes médicales et l'armée vont alors s'organiser pour mettre au point des protocoles thérapeutiques et des mesures prophylactiques efficaces. Certes, tous ces efforts seront récompensés et l'amputation du membre gangrené ne sera plus systématique. Néanmoins, pendant cette guerre de 1914-1918, une arme thérapeutique essentielle et réellement efficace manque encore aux soldats de la santé : l'antibiothérapie.
A Comparative Study of White and Black American Soldiers during the First World War
Authors: Keene Jennifer
Published: December 2016

Résumé Quand on compare les expériences des soldats blancs et des soldats noirs dans l'armée américaine pendant la Première Guerre mondiale, on voit immédiatement que les mesures racistes appliquées par les autorités américaines ont, au-delà des soldats noirs, atteint l'armée elle-même. Un pourcentage plus élevé des Noirs américains ont été enrôlés et sont morts de maladies. Mais parce qu'ils ne constituaient que 3 % des forces combattantes, ils ont été peu nombreux à mourir au combat. La volonté de former les régiments par race, de déplacer la plupart des soldats noirs dans les services auxiliaires, et de s'assurer que la majorité des soldats dans chaque camp d'entraînement étaient blancs, a aussi eu des conséquences pour les soldats blancs. L'armée américaine a abandonné le principe des unités régionales et a fait porter le poids de la guerre en priorité sur les soldats blancs. Il est possible que l'armée américaine ait été moins efficace sur les champs de bataille parce qu'elle n'a pas voulu utiliser les capacités des Noirs américains à combattre et à commander.
Populations et économies des colonies d'implantation européenne en Afrique (Afrique du Sud, Algérie, Kenya et Rhodésie du Sud)
Authors: Lutzelschwab Claude
Published: December 2016

Résumé L’établissement de colons européens dans l’agriculture tempérée fut fortement tributaire de l’importance relative des populations autochtones, c’est-à-dire de leur densité démographique. En Afrique, quelques territoires devinrent des terres d’émigration pour les Européens, dès la fin du xvii e siècle en Afrique du Sud, à partir des années 1830 en Algérie, plus tardivement, au xx e siècle en Rhodésie du Sud et au Kenya. Cet article examine les modalités de colonisation de ces territoires où les Européens s’installèrent sur la terre et entrèrent en concurrence directe avec les producteurs indigènes, tout en ne constituant qu’une faible fraction de la population totale. La nécessité de composer avec la population indigène a entraîné l’intervention du législateur colonial, afin de modifier l’accès des différents groupes sociaux (indigènes et européens) aux facteurs de production (au sens large).
Principles and Prospects of the Life Course Paradigm
Authors: Kok Jan
Published: December 2016

Résumé La démographie historique semble avoir pris un tournant « micro » en se concentrant de plus en plus sur l’analyse des parcours de vie. Si l’on suit ses avocats, il ne s’agit de rien moins que d’un nouveau paradigme de la démographie (historique). Cet article propose une vue critique de cette affirmation, en examinant les succès en termes de recherche et en discutant les obstacles potentiels à la réussite des promesses de cette nouvelle approche. L’adoption de l’analyse des parcours de vie a déjà fourni des contributions très neuves par rapport aux sujets ignorés de la démographie historique traditionnelle (les orphelins, le service domestique dans le cycle de vie, les études comparées sur les dynamiques familiales). Des sujets comme le vieillissement, les migrations et la fécondité ont également bénéficié de la collecte et de l’analyse des données du parcours de vie. En dépit de ces avancées, le développement de cette approche peut être compromis par plusieurs facteurs : le concept lui-même, les méthodes statistiques utilisées et les pratiques de recherches dominantes ainsi que l’attraction de notre champ. Tout d’abord l’affirmation de la capacité d’organiser sa propre vie est d’application difficile dans les recherches historiques. Néanmoins, l’ignorance des motifs et des buts des individus ne devrait pas dissuader d’identifier quels étaient les plus probables dans certains lieux et certaines périodes. Ensuite, la méthode de l’« event history analysis » ne permet pas de clarifier les parcours de vie en tant que processus. Des modèles plus élaborés devraient permettre de préciser l’impact des expériences passées, des conduites alternatives, des interactions entre les processus et les contextes. Enfin, le coût d’apprentissage de la démographie historique risque de devenir trop élevé, en particulier si des techniques encore plus poussées doivent être utilisées. Des équipes interdisciplinaires pourraient résoudre cette difficulté. Par ailleurs, l’approche du parcours de la vie suppose des bases de données compliquées et très riches. Tout cela ne peut être accompli par les équipes universitaires traditionnelles et les chercheurs solitaires. Dans ce domaine, les pratiques de recherche (et d’apprentissage) doivent s’orienter vers le partage de données, la collaboration et l’exploitation de banques de données publiques. Finalement, afin d’attirer les chercheurs d’autres domaines, la recherche doit privilégier des questions à fort enjeu politique aujourd’hui comme le niveau de la fécondité (enjeu du remplacement), les migrations et l’intégration des populations étrangères.
Transatlantic Anxieties: New York's Nineteenth-Century Foundling Asylums and the London Foundling Hospital
Authors: Miller Julie
Published: December 2016

Résumé Dans les années 1850, la ville de New York fit face à une croissance du nombre d’enfants abandonnés. À la recherche de solutions, les responsables municipaux prirent l’hospice des enfants abandonnés de Londres comme modèle. Le fait que cette dernière institution concentrait son action sur la récupération des femmes perdues les séduisait, car cela faisait écho à leur perception angoissée de la situation à New York, qui, selon eux, se transformait en une « ville d’étrangers » où l’ordre social explosait. Un de ces responsables, Isaac Townsend, estimait même que les fameux programmes musicaux et artistiques de l’hospice londonien élevaient le niveau moral et culturel des habitants de la capitale anglaise. Il espérait reprendre ces programmes culturels dans l’asile des enfants abandonnés que la ville de New York projetait de construire. New York construisit effectivement un hospice, nommé Infant’s Home et rattaché au Nursery and Child’s Hospital. Celui-ci, ainsi que trois autres institutions du même type (le New York Infant Asylum, le New York Foundling Asylum et le Randall’s Island Infant Hospital), ouvrit après la guerre de Sécession. Mais il s’avéra impossible de se conformer totalement aux méthodes du modèle londonien. La décentralisation de la politique d’aide sociale, la séparation des Églises et de l’État aux États-Unis, la concurrence entre protestants et catholiques, les tensions entre les immigrants et les mouvements nativistes, les combinaisons politiques, la difficulté de trouver des nourrices autour de New York, et même le désintérêt des New-Yorkais pour les arts, furent autant d’éléments qui expliquèrent cette incapacité. Ainsi, malgré son héritage londonien, New York géra la question des enfants abandonnés selon des logiques qui reflétaient des sensibilités locales et nationales propres vis-à-vis de l’assistance aux pauvres, de la religion, de la politique, et ceci, en définitive, aboutit à un écart net par rapport au modèle londonien.
L'ascension sociale des jeunes filles de l'assistance publique (1880-1940)
Authors: Jablonka Ivan
Published: December 2016

Résumé Sous la Troisième République, l’Assistance publique maintient autoritairement les pupilles à la terre et les enfants assistés sont massivement gagés dans les fermes à l’âge de treize ans. Par la suite, les garçons réussissent peu ou prou à s’émanciper, notamment grâce au service militaire et au travail en usine. Les filles, en revanche, paraissent bloquées : mal instruites, peu diplômées, confinées aux tâches ingrates de la domesticité agricole ou bourgeoise, elles connaissent un destin professionnel assez terne, quand elles n’arrêtent pas tout simplement de travailler après le mariage. À partir de la première guerre mondiale, le refus de demeurer dans l’agriculture s’accuse chez les filles de l’Assistance publique et un réel désir d’ascension sociale se fait jour. Elles accèdent alors aux métiers qui se sont féminisés dès la fin du xix e siècle (enseignement, postes et télécommunications, emplois de bureau, etc.). Mais elles n’utilisent pas nécessairement le diplôme pour s’élever socialement ; elles comptent aussi avec l’expérience professionnelle acquise « sur le tas », les migrations et le mariage.