bluuebunny/crossref_metadata_2025 huggingface dataset:
FECHAMENTO DO APÊNDICE ATRIAL ESQUERDO
Authors: Rocha Débora Freire Ribeiro , Amaral Leonardo Veloso do , Prudente Maurício Lopes , Guimarães Henrique Lima , Fernandes Fernando Henrique , Araújo Adriano Gonçalves de , Silva João Batista Masson , Gardenghi Giulliano
Published: November 2024

Pessoas com fibrilação atrial (FA) tem um risco cinco vezes maior de sofrer um AVC do que as pessoas que não sofrem esse problema. O acidente vascular cerebral secundário à FA tem sido associado a taxas de mortalidade e de incapacidade permanente elevadas, porquanto sua prevenção eficaz é importante. Métodos mecânicos para a oclusão do AAE foram desenvolvidos como alternativa à anticoagulação oral para pacientes com contraindicações ou complicações derivadas da anticoagulação. O caso é de um paciente do sexo masculino, de 86 anos, hipertenso e portador de FA que foi admitido em nosso serviço no dia 07/06/2020 com quadro de lipotimia, dispneia e dor torácica associado a bradicardia (FC de 32 bpm) e ritmo de bloqueio atrioventricular total com FA, foi internado na UTI, passado um marcapasso provisório transvenoso, suspenso o atenolol e iniciado anticoagulação plena com enoxaparina. No entanto evoluiu com quadro de melena importante no dia 12/06/2020 com queda hematimétrica e necessidade de transfusão sanguínea, sendo suspensa a anticoagulação e realizada investigação com EDA e colonoscopia. Foi submetido a ecocardiograma transesofágico e estudo eletrofisiológico para avaliar cardioversão e ablação da FA. Foram realizadas duas tentativas de cardioversão elétrica sem sucesso. Paciente recebe alta hospitalar no dia 21/06/2020 em uso de Eliquis 5mg 2x ao dia associado a clopidogrel. Porém no dia 06/07/2020 evoluiu com hematoma contido em hemitórax direito retropeitoral, foi reduzido a dose do Eliquis® para 2,5mg 2x ao dia, paciente manteve persistência de hematoma sendo então suspenso o anticoagulante e programado o fechamento de AAE.
SÍNDROME DO ROUBO CORONÁRIO-SUBCLÁVIO COMO CAUSA DE ANGINA INSTÁVEL
Authors: Demuner Patricia Ferreira , Rodrigues Débora , Amaral Leonardo Veloso do , Vale Georges Ferreira do , Souza Fábio Henrique Ribeiro de , Nery Max Weyler , Prudente Mauricio Lopes , Gardenghi Giulliano
Published: November 2024

A síndrome do roubo coronário-subclávio é uma condição rara, associada a pacientes submetidos a cirurgia de revascularização miocárdica com enxerto mamário. Neste contexto apresenta-se como um diagnóstico diferencial de angina, que quando corretamente diagnosticado e tratado pode melhorar o desfecho e evitar as potenciais complicações. Relato do caso: Paciente do sexo masculino, 65 anos, hipertenso, dislipidêmico, doença arterial periférica e coronariana submetido a cirúrgica de revascularização miocárdica no ano de 2000 com enxerto mamário em descendente anterior. Estava em acompanhamento cardiológico regular, assintomático do ponto de vista cardiovascular. Neste primeiro momento foram realizados exames de prova isquêmica, cuja cintilografia demonstrou carga isquêmica de 8% e indicado cateterismo com subclávia com lesão de 70% na origem e enxerto mamário com patência preservada. Cerca de 6 meses após esta consulta, paciente retorna com queixa de angina estável. Realizada nova cintilografia cujo carga isquêmica havia aumentado, agora de 12%. Neste momento indicado tratamento percutâneo da lesão de subclávia, utilizando stent balão-expansível de 9,0x25mm com sucesso, realizado controle angiográfico com cateter PigTail demonstrando bom resultado. No retorno ambulatorial do paciente apresentava melhora substancial dos sintomas anginosos, confirmados em cintilografia com redução da carga isquêmica para 5%. Conclusão: O relato acima descreve um quadro clássico de síndrome do roubo da subclávia, com apresentação de precordialgia, mostrando que o rápido diagnóstico dessa rara condição e o devido tratamento têm potencial de melhorar o quadro clínico e a perfusão miocárdica.
TUMOR DE BRENNER BENIGNO DO OVÁRIO
Authors: Luciano Ana Luíza Fleury , Sousa André Maroccolo de , Souza Liliane Cândida de Paula , Rocha Rogério Cândido , Pinto Sebastião Alves , Sousa Juarez Antônio de
Published: November 2024

Os tumores de Brenner surgem do epitélio ovariano e são classificados pela Organização Mundial de Saúde (OMS) como benignos, malignos e boderline. São caracterizados por um ninho de células do tipo transicionais, as quais se assemelham às uroteliais, envolto por um estroma fibroso. Apresentam-se, geralmente, em pacientes entre a quinta e a sétima década de vida. São, em sua maioria, assintomáticos e descobertos acidentalmente, através da detecção de uma massa pélvica ao exame físico, exames de imagem, laparotomia, ou mesmo no estudo patológico de uma ooforectomia realizada por outros motivos. Em 25% dos casos, estes tumores são associados a presença concomitante de outros tipos de tumores, sendo mais comuns os cistoadenomas.
DIABETES GESTACIONAL
Authors: Saidah Mohamed Kassem , Saidah Tárik Kassem , Evangelista Patrícia Gonçalves , Amaral Waldemar Naves do
Published: November 2024

O objetivo deste estudo é trazer uma revisão bibliográfica atualizada sobre a diabetes gestacional do conceito ao diagnóstico e descrever a importância do conhecimento, atitude e autocuidado em gestante diabética. Diabetes gestacional é aquele diagnosticado durante a gravidez em uma paciente que não foi diagnosticada com diabetes antes da gravidez no qual chamamos de diabetes prévia. O diagnóstico é controverso, porém recomenda-se que por ocasião da primeira consulta pré-natal, todas as grávidas deverão ser submetidas a uma glicemia plasmática em jejum. A falta de consciência, atitudes negativas e práticas inadequadas de autocuidado entre pacientes diabéticos, são algumas das variáveis importantes que influenciam a progressão do diabetes e suas complicações, as quais são amplamente evitáveis através da educação e do envolvimento do paciente. O diabetes gestacional está associado a graves doenças maternas, fetais e neonatais. O pré-natal é uma oportunidade para mulheres grávidas para receber orientações, elas devem ser informadas sobre os seus cuidados com a saúde, a importância de exercícios regulares, ajuste da dieta e adequação a tomada de medicamentos melhorando assim os conhecimentos, atitudes e autocuidado em gestantes diabéticas. A literatura sobre conhecimento, atitude e autocuidado sobre o DMG em mulheres grávidas é escassa.
UVEÍTE INTERMEDIÁRIA SECUNDÁRIA À COVID-19
Authors: Sobrinho Vinicius Stival Veneziano , Pereira Augusto , Neto Francisco Dias Lucena
Published: November 2024

Objetivo: compartilhar um caso de uveíte intermediária, pós infecção da fase aguda, imunomediada pela SARS-CoV-2, documentando a capacidade de apresentação clínica multiforme desta infecção. Materiais e método: relato de caso, propedêutica armada e exames de imagem, com revisão de literatura bibliográfica. Resultados: Um homem, de 50 anos, com Reação de Cadeia Polimerase (PCR) positivo em swab nasal para SARS-COV-2, 10 dias após isolamento, queixou-se de baixa acuidade visual e embaçamento visual bilateral. Vitreíte em ambos os olhos, 2+/4 em OD e 1+/4+ em OE e haze vítreo foram documentados em retinografia simples. 15 dias após o diagnóstico precoce e o início do tratamento, o paciente evoluiu com melhora de acuidade visual. Na reavaliação da biomicroscopia e fundoscopia, houve melhora do padrão da vitreíte. Conclusões: a paciente negou história médica de doenças crônicas autoimunes, inflamatórias e foi realizada a exclusão de possíveis etiologias através das principais sorologias. A clássica apresentação clínica, diagnóstico precoce e resposta clínica, com redução gradual e resposta satisfatória falam a favor de uma uveíte intermediária. Apresentamos este caso de envolvimento ocular, dias após a uma condição inflamatória sistêmica por COVID - 19, para documentar a extraordinária e multifacetada capacidade de manifestação clínica viral.
OCLUSÃO DE FORAME OVAL PATENTE PÓS INFARTO DO MIOCÁRDIO POR EMBOLIA ARTERIAL CORONARIANA
Authors: Guimarães Ghiordana Milena Dias Lopes , Guimarães Henrique Lima , Silva João Batista Masson , Gardenghi Giulliano , Prudente Maurício Lopes , Barbosa Flávio Passos
Published: November 2024

O forame oval patente é uma cardiopatia congênita prevalente em cerca de 30% da população adulta e está associado na gênese de eventos cerebrovasculares isquêmicos, oclusões arteriais periféricas, e menos comumente, com a síndrome coronariana aguda. A embolia arterial coronariana paradoxal é considerada rara, sendo uma causa subdiagnosticada de infarto agudo do miocárdio em pacientes com perfil de baixo risco para doença coronariana. Relatamos um caso de infarto agudo do miocárdio com supradesnivelamento do segmento ST de parede anterior por embolia paradoxal presumida com posterior oclusão por via percutânea do forame oval patente.
INFECÇÃO CONGÊNITA POR CITOMEGALOVÍRUS
Authors: Carneiro Luciana Zendron
Published: November 2024

O citomegalovírus (CMV) é um vírus que pode causar transmissão vertical. As mulheres grávidas podem ser afetadas por uma infecção primária ou secundária à reativação ou reinfecção. Após uma infecção primária ou vírus, pode tornar-se latente em células brancas com reativações periódicas e há também a possibilidade de reinfecção com uma nova cepa visto que uma infecção inicial não garante a imunidade cruzada. Recém-nascidos (RN) portadores de CMV podem ser acometidos no futuro por distúrbios neurológicos na infância e surdez. No presente trabalho, apresentamos um relato de caso de RN do sexo masculino com provável infecção por CMV cuja mãe apresentava exames compatíveis à imunidade ao vírus. Isto abre possibilidades de discutir outras formas de transmissão para o conceito de gestante previamente imune.
INTERVENÇÃO CORONÁRIA PERCUTÂNEA EM OCLUSÃO TOTAL CRÔNICA (CTO)
Authors: Rocha Débora Freire Ribeiro , Guimarães Henrique Lima , Lopes Maurício Prudente , Barbosa Flavio Passos , Morais Júnior Álvaro de , Gardenghi Giulliano
Published: November 2024

A intervenção coronária percutânea (ICP) de alto risco (CHIP-PCI) refere-se à revascularização percutânea clinicamente orientada de pacientes com doença arterial coronariana (DAC) extensa. Requer um conjunto de habilidades, pessoal, equipamentos e suporte logístico além daqueles necessários para ICP convencional. A ICP em oclusão total crônica (CTO) é um campo da cardiologia intervencionista em expansão. Apesar disso, a ICP-CTO corresponde a apenas 10% do total de procedimentos. As diretrizes atuais recomendam que a ICP de CTO deve ser considerada para redução de isquemia no território miocárdico correspondente e/ou para redução de angina. Neste trabalho, descreveremos um caso de uma CHIPPCI em um paciente coronariopata sintomático portador de múltiplas comorbidades e alto risco cirúrgico.
RELATO DE CASO DE EDEMA AGUDO DE PULMÃO POR MOVIMENTO ANTERIOR SISTÓLICO APÓS LIPOASPIRAÇÃO
Authors: Melo Silva Mateus Moreira de , Gundim Daniel Ferreira , Souza Fabrício Rodrigues de , Gardenghi Giulliano , Elmiro Gustavo Siqueira
Published: November 2024

O movimento anterior sistólico é a movimentação de um ou mais folhetos da válvula mitral na direção anterior, ocasionando obstrução durante a saída do conteúdo sistólico do ventrículo esquerdo. O diagnóstico pode demandar ecocardiografia transesofágica ou ressonância magnética e seu tratamento é principalmente clínico. O objetivo desse texto é relatar um caso desafiador no pós-operatório de cirurgia plástica, que cursou com clínica de edema agudo de pulmão e recebeu diagnóstico posterior de Movimento Anterior Sistólico, o que levou a necessidade de medidas particularizadas, contrastantes as medidas tomadas baseadas no diagnóstico primário inespecífico.
INSUFICIÊNCIA CARDÍACA AGUDA SECUNDÁRIA À DOENÇA TRIARTERIAL CORONARIANA GRAVE EM INDIVÍDUO JOVEM E ALTERAÇÃO DA LIPOPROTEÍNA A
Authors: Canedo Fernando Araujo Cintra , Oliveira Larissa Xavier Alves de , Marçal Paula Chiavenato , Perillo Filho Marcos Pinto , Nery Max Weyler , Gardenghi Giulliano
Published: November 2024

A doença arterial coronariana aterosclerótica é pontuada como a principal causa de insuficiência cardíaca aguda e crônica no mundo. Quando avaliamos a fundo os fatores de risco modificáveis e não modificáveis para aterosclerose, nos deparamos com escores de risco cardiovascular global, que delimitam metas preventivas e posteriormente terapêuticas, com o objetivo de reduzir a morbimortalidade por doenças cardiovasculares. O presente relato de caso nos evidencia uma doença coronariana grave, com aterosclerose difusa, em um paciente com escore de risco global baixo e alteração de lipoproteína A (LpA), levantando questionamentos sobre o aprimoramento de medidas para reestratificação global de risco cardiovascular.
SÍFILIS CONGÊNITA E FATORES ASSOCIADOS EM ANÁPOLIS – GOIÁS, 2017-2021
Authors: Mendes Neto Rhayanne Claudine , Emídio Izaura Costa Rodrigues
Published: November 2024

Sífilis congênita é um caso epidemiológico de progressão crescente ao longo dos anos. Notificações de casos confirmados de sífilis congênita são reportados com frequência em aspectos mundiais. A região Centro-Oeste possui literatura escassa associada à descoberta de parâmetros epidemiológicos. Com isso, o principal objetivo deste trabalho é identificar a prevalência e os fatores associados à sífilis congênita no município de Anápolis – Goiás, entre os anos de 2017 a 2021. Uma curva côncava foi descoberta neste período, evidenciando um aumento progressivo e posterior decaimento progressivo, ao longo dos anos estudados, para a região Centro-Oeste. Estes resultados mostraram um lugar de destaque para a região de Anápolis (terceiro lugar), dentre todas as demais cidades estudadas da região Centro-Oeste. Apesar de apresentar resultados, mais estudos sobre a cidade de Anápolis são necessários para explorar conhecimentos epidemiológicos acerca da região.
RELATO DE CASO DE UM MUTIRÃO PEDIÁTRICO DE ATENDIMENTO SEMIPRESENCIAL NA CIDADE DE SILVÂNIA-GOIÁS
Authors: Barros Giselle Pulice , Lopes Filho Marcus Vinicius Lobo
Published: November 2024

Trata-se de um relato de caso de um mutirão em pediatria, de atendimento semipresencial, na cidade de Silvânia, localizada no Estado de Goiás, para demonstração do método de consultas semipresenciais criado pela startup médica medicou.net à população.
PERFIL DE MULHERES SUBMETIDAS A CURETAGEM UTERINA EM UMA MATERNIDADE PÚBLICA
Authors: Santos Ludmira Fortuna , Carvalho Laura Araújo de , Poloniato Thays Barbieri , Souza Guerra Lazaro Edson Lemes de , Amaral Waldemar Naves do
Published: November 2024

Introdução: Na assistência à saúde da mulher, algumas condições indicam o esvaziamento da cavidade uterina, em caso de suspeita de retenção dos tecidos placentários parto e para o tratamento de abortamento. Objetivo: Descrever as indicações e o perfil das mulheres submetidas a curetagem uterina. Método: Estudo de natureza observacional com delineamento transver-sal, descritivo e de abordagem quantitativa, com coleta secundária de dados em prontuário físico/eletrônico entre os meses de janeiro a julho 2022, realizado no Hospital e Materni-dade Dona Iris. Os dados foram inseridos no software estatístico planilha eletrônica Mi-crosoft Office Excel, aplicou-se estatísticas simples com frequência absoluta e relativa. Resultados: Do total de mulheres submetidas ao procedimento de esvaziamento da cavi-dade uterina devido a retenção de tecidos placentários, 82% deveram-se a abortamentos, destas, 74% foram encaminhadas à curetagem uterina e 8% à Aspiração Manual Intraútero (AMIU). Identificou-se como relevante neste estudo as variáveis sociodemográficas faixa etária de 20 a 39 anos (84%), não viver com parceria (72%) e ter ensino médio completo (56%). Conclusão: Observou-se a curetagem uterina como principal método adotado para o esvaziamento uterino em decorrência de abortamento, mulheres em idade fértil, multípa-ras, sem parceria e baixa adesão ao pré-natal. Sugere-se ações de atenção ao abortamento, em especial a educação acerca do uso dos métodos disponíveis.
CIRURGIA CARDÍACA MINIMAMENTE INVASIVA PARA SUBSTITUIÇÃO DE BIOPRÓTESE AÓRTICA IMPLANTADA POR VIA TRANSCATETER APÓS DEGENERAÇÃO PRECOCE
Authors: Alcântara Borges Larissa Manzan de , Gardenghi Giulliano , Pansani João Alberto , Loyola Stanlley de Oliveira , Elmiro Gustavo Siqueira , Souza Artur Henrique de
Published: November 2024

A substituição cirúrgica de uma prótese valvar aórtica implantada por via transcateter (TAVI) que apresentou degeneração precoce (em menos de 24 meses após seu implante) não ocorre comumente em curto espaço de tempo e pode estar relacionada a pior prognóstico e complicações. A cirurgia cardíaca minimamente invasiva pode minimizar o estresse cirúrgico em situações em que ocorra fragilidade do indivíduo submetido. O presente artigo tem por finalidade realizar uma revisão do tema e descrever um caso de uma paciente de 84 anos, frágil, que apresentou disfunção valvar após TAVI e foi submetida a substituição cirúrgica da bioprótese, por meio de cirurgia minimamente invasiva.
Evaluating the colour stability of esthetic resin composite: A study of Neospectra ST under different staining conditions
Authors: Kondipudi Nimisha , Palla Likhitha , Borugadda Roopesh , Neelima U Lavanya , Manchem Aishwarya , A K Nawaz Mohammad
Published: November 2024

Background:There is a burgeoning interest in the colour permanence of aesthetic restorations, although only a handful of studies have been documented thus far.Aim:To investigate the impact of various common staining solutions on nanohybrid composite resin..Materials and methods:Forty disk-shaped specimens (10 X 2 mm) were fabricated with Neo SpectraST composite material. The specimens were divided into four groups with 10 specimens (n=10) in each, based on the staining solutions, Group I: Turmeric, Group II: Coffee, Group III: Coke, and Group IV: Distilled water. Baseline measurements were taken using an ultraviolet spectrophotometer. Each sample group was immersed in their respective staining solutions, and the colour changes were recorded after 1, 7, and 14 days of immersion using the same spectrophotometer. The absorption values were recorded within the 300 to 800 nm range at baseline and after the immersion. The data was collected and subjected to statistical analysis.Results:Neo spectra ST composite showed the maximum staining capacity with the turmeric group compared to otherstaining solutions. One-way ANOVA showed significant differences (p=0.000) among the staining solutions at different time intervals. Repeated measures ANOVA displayed significant differences within the staining solutions (Turmeric: p=0.005; Coffee: p=0.001; and Coke: p=0.001) at different time intervals.Conclusion:The nanohybrid composite resin showed a significant colour change to turmeric compared to other staining solutions.
Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Caputo Miranda , Chandar Rupali , Mok Angus , Linden Sean , Goudfrooij Paul , Whitmore Bradley C.
Published: November 2024

Observations of young star clusters in a variety of galaxies have been used to constrain basic properties related to star formation, such as the fraction of stars found in clusters (Γ) and the shape of the cluster mass function (CMF). However, the results can depend heavily on the reliability of the cluster age-dating process and other assumptions. One of the biggest challenges for successful age-dating lies in breaking the age–reddening degeneracy, where older, dust-free clusters and young, reddened clusters can have similar broadband colors. While this degeneracy affects cluster populations in all galaxies, it is particularly challenging in systems with dusty, extreme star-forming environments. We study the cluster demographics in the luminous infrared galaxy NGC 1614 using Hubble Space Telescope imaging taken in eight optical–near-infrared passbands. For age-dating, we adopt a spectral energy distribution fitting process that limits the maximum allowed reddening by region and includes Hα photometry directly. We find that without these assumptions essentially all clusters in the dust-free UV-bright arm that should have ages ≈50–250 Myr are incorrectly assigned ages younger than 10 Myr. We find that this method greatly reduces the number of clusters in the youngest (τ < 10 Myr) age bin and shows a fairly uniform distribution of massive clusters, the most massive being ≈few × 107
M
⊙. A maximum likelihood fit shows that the CMF is well fitted by a power law with an index of approximately −1.8, with no statistically significant high-mass cutoff. We calculate the fraction of stars born in clusters to be Γ1−10 = 22.4% ± 5.7%. The fraction of stars in clusters decreases quickly over time, with Γ10−100 = 4.5% ± 1.1% and Γ100−400 = 1.7% ± 0.4%, suggesting that clusters dissolve rapidly over the first ∼0.5 Gyr. The decreasing fraction of stars in clusters is consistent with the declining shape observed for the cluster age distribution.
The Discovery and Evolution of a Radio Continuum and Excited-OH Spectral-line Outburst in the Nearby Galaxy NGC 660
Authors: Salter C. J. , Ghosh T. , Minchin R. F. , Momjian E. , Catinella B. , Lebron M. , Lerner M. S.
Published: November 2024

Arecibo 305 m Telescope observations between 2008 and 2018 detected a radio continuum and spectral-line outburst in the nearby galaxy, NGC 660. Excited-OH maser emission/absorption lines near 4.7 GHz, and H2CO absorption at 4.83 GHz varied on timescales of months. Simultaneously, a continuum outburst occurred in which a new compact component appeared, with a GHz-peaked spectrum and a 5 GHz flux density that rose to a peak value of about 500 mJy from 2008.0 to 2012.0. Follow-up interferometric continuum images from the Very Large Array at 10 GHz of this new continuum component determined it to be located at the nucleus of NGC 660. Subsequent High Sensitivity Array line and continuum very long baseline interferometry observations of the NGC 660 nucleus revealed a morphology that appears to be consistent with rapidly precessing, mildly relativistic jets from the central black hole. While requiring detailed modeling, this strongly suggests that the outburst is due to nuclear activity. From its timescale, the shape of the continuum light curve, and the milliarcsec radio structure, the most likely cause of the outburst is active galactic nuclei-type activity of accretion of a gas cloud onto the central black hole.
Extinction of Taurus, Orion, Perseus and California Molecular Clouds Based on the LAMOST, 2MASS, and Gaia Surveys. II. The Extinction Law
Authors: Cao 曹 ZheTai 哲泰 , Jiang 姜 Biwei 碧沩 , Wang 王 Shu 舒 , Li 李 Jun 军
Published: November 2024

The extinction law from ultraviolet (UV) to infrared (IR; 0.2–24 μm) is determined by relying on the blue-edge method and color-excess ratios for some nearby molecular clouds, from the low-mass star-forming region to the massive star-forming region. The observational data are collected from nine photometric surveys, along with stellar parameters from the Apache Point Observatory Galaxy Evolution Experiment and LAMOST spectroscopic surveys. Within the uncertainties, the optical ratio of selective to total extinction (

R

G

BP

) does not vary substantially across the clouds, irrespective of the density, specifically

R

G

BP

=
2.302
±
0.027

, where

R

G

BP

≡

A

G

BP

/

E

G

BP

,

G

RP

. The IR extinction law is consistent with Wang & Chen. The extinction law in the UV band is compromised by the shallow depth with A
V ≤ 2 mag and is hard to describe by one parameter R. In addition, the extinction in the WISE/W1 band is significantly larger than in the Spitzer/IRAC1 band in the dense regions, which is attributed to the ice water absorption.
Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Park Minjung , Belli Sirio , Conroy Charlie , Johnson Benjamin D. , Davies Rebecca L. , Leja Joel , Tacchella Sandro , Mendel J. Trevor , Benton Chloë , Bugiani Letizia , Emami Razieh , Khoram Amir H. , Li Yijia , Maheson Gabriel , Mathews Elijah P. , Naidu Rohan P. , Nelson Erica J. , Terrazas Bryan A. , Weinberger Rainer
Published: November 2024

Massive quiescent galaxies in the young Universe are expected to be quenched rapidly, but it is unclear whether they all experience starbursts before quenching and what physical mechanism drives rapid quenching. We study 14 massive quiescent galaxies (

log
(

M

⋆

/

M

⊙

)
>
10

) at z ∼ 2 selected from a representative sample of the Blue Jay survey. We reconstruct their star formation histories (SFHs) by fitting spectral energy distribution models to the JWST/NIRSpec R ∼ 1000 spectra. We find that massive quiescent galaxies can be split into three categories with roughly equal numbers of galaxies according to their SFHs: (1) relatively old galaxies quenched at early epochs; (2) galaxies that are rapidly and recently quenched after a flat or bursty formation history (depending on the assumed prior); and (3) galaxies that are rapidly and recently quenched after a major starburst. Most recently quenched galaxies show neutral gas outflows, probed by blueshifted Na i D absorption, and ionized gas emission, with line ratios consistent with active galactic nucleus (AGN) diagnostics. This suggests that AGN activity drives multiphase gas outflows, leading to rapid quenching. By tracing back the SFHs of the entire sample, we predict the number density of massive quiescent galaxies at z = 4–6: n = (1.5–6.0) × 10−5 Mpc−3. The two old massive quiescent galaxies in our sample appear to have extremely early formation and quenching (z ≳ 6) and are possibly descendants of early post-starbursts at z > 3. These galaxies still show neutral gas reservoirs and weak Hα emission, perhaps because the ejective AGN feedback that caused rapid quenching has weakened over time.
Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Srinivasaragavan Gokul P. , Yang Sheng , Anand Shreya , Sollerman Jesper , Ho Anna Y. Q. , Corsi Alessandra , Cenko S. Bradley , Perley Daniel , Schulze Steve , Sanchez-Fleming Marquice , Pope Jack , Sarin Nikhil , Omand Conor , Das Kaustav K. , Fremling Christoffer , Andreoni Igor , Bruch Rachel , Burdge Kevin B. , De Kishalay , Gal-Yam Avishay , Gangopadhyay Anjasha , Graham Matthew J. , Jencson Jacob E. , Karambelkar Viraj , Kasliwal Mansi M. , Kulkarni S. R. , Martikainen Julia , Sharma Yashvi S. , Tzanidakis Anastasios , Yan Lin , Yao Yuhan , Bellm Eric C. , Groom Steven L. , Masci Frank J. , Nir Guy , Purdum Josiah , Smith Roger , Sravan Niharika
Published: November 2024

We study a magnitude-limited sample of 36 broad-lined type Ic supernovae (SNe Ic-BL) from the Zwicky Transient Facility Bright Transient Survey (detected between 2018 March and 2021 August), which is the largest systematic study of SNe Ic-BL done in literature thus far. We present the light curves (LCs) for each of the SNe and analyze the shape of the LCs to derive empirical parameters, along with the explosion epochs for every event. The sample has an average absolute peak magnitude in the r band of

M

¯

r
,
max

=
−
18.51
±
0.15

mag. Using spectra obtained around peak light, we compute expansion velocities from the Fe ii 5169 Å line for each event with high enough signal-to-noise ratio spectra, and find an average value of

v
ph

¯

=
16
,
100
±
1100

km s−1. We also compute bolometric LCs, study the blackbody temperature and radii evolution over time, and derive the explosion properties of the SNe. The explosion properties of the sample have average values of

M

¯

Ni

=

0.37

−
0.06

+
0.08

M

⊙

,

M

¯

ej

=

2.45

−
0.41

+
0.47

M

⊙

, and

E

¯

K

=

(

4.02

−
1.00

+
1.37

)

×

10

51

erg. Thirteen events have radio observations from the Very Large Array, with eight detections and five non-detections. We find that the populations that have radio detections and radio non-detections are indistinct from one another with respect to their optically inferred explosion properties, and there are no statistically significant correlations present between the events’ radio luminosities and optically inferred explosion properties. This provides evidence that the explosion properties derived from optical data alone cannot give inferences about the radio properties of SNe Ic-BL and likely their relativistic jet formation mechanisms.
The Radio Halo in PLCKESZ G171.94–40.65: Beacon of Merging Activity
Authors: Santra R. , Kale R. , Giacintucci S. , Wik D. R. , Venturi T. , Dallacasa D. , Cassano R. , Brunetti G. , Joshi D. C.
Published: November 2024

We present the first multifrequency analysis of the candidate ultrasteep spectrum radio halo in the galaxy cluster PLCKESZ G171.94−40.65, using the upgraded Giant Metrewave Radio telescope (400 MHz), and Karl G. Jansky Very Large Array (1–2 GHz) observations. Our radio data have been complemented with archival Chandra X-ray observations to provide a crucial insight into the complex intracluster medium physics, happening at large scales. We detect the radio halo emission to the extent of ∼1.5 Mpc at 400 MHz, significantly larger than previously reported, along with five tailed galaxies in the central region. We also report the discovery of an unknown diffuse source “U,” at the cluster periphery, with an extent of 300 kpc. Using the available observations, we have found that the radio spectrum of the halo is well-fitted with a single power law, having a spectral index of −1.36 ± 0.05, indicating that it is not an ultrasteep spectrum radio halo. Our low-resolution (25″) resolved spectral map shows an overall uniform spectral index, with some patches of fluctuations. The X-ray and radio surface brightness are morphologically cospatial, with a slight extension along the northwest–southeast direction, seen in both maps. The radio and X-ray surface brightness indicates strong positive correlations, with sublinear correlation slopes (∼0.71). Multiple tailed galaxies and the radio halo indicate a high dynamical activity at the cluster central region.
Unveiling the Progenitors of a Population of Likely Peculiar Gamma-Ray Bursts
Authors: Zhu Si-Yuan , Tam Pak-Hin Thomas
Published: November 2024

Traditionally, gamma-ray bursts (GRBs) are classified as long and short GRBs, with T
90 = 2 s being the threshold duration. Generally, long-duration GRBs (LGRBs; T
90 > 2 s) are associated with the collapse of massive stars, and short-duration (SGRBs; T
90 < 2 s) are associated with compact binary mergers involving at least one neutron star. However, the existence of a population of so-called “peculiar GRBs”—i.e., LGRBs originating from mergers or long Type I GRBs, and SGRBs originating from collapsars or short Type II GRBs—has challenged the traditional paradigm of GRB classification. Finding more peculiar GRBs may help to give more insight into this issue. In this work, we analyze the properties of machine-learning-identified long Type I GRB and short Type II GRB candidates, long GRBs-I and short GRBs-II (the so-called “peculiar GRBs”). We find that long GRBs-I almost always exhibit properties similar to Type I GRBs, which suggests that mergers may indeed produce GRBs with T
90 > 2 s. Furthermore, according to the probability given by the redshift distribution, short GRBs-II almost exhibit properties similar to Type II GRBs. This suggests that the populations of short Type II GRBs are not scarce and that they are hidden in a large number of samples without redshifts, which is unfavorable for the interpretation that the jet progression leads to a missed main emission.
AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817*
Authors: Netzer Hagai , Goad Michael R. , Barth Aaron J. , Cackett Edward M. , Horne Keith , Hu Chen , Kara Erin , Korista Kirk T. , Kriss Gerard A. , Lewin Collin , Montano John , Arav Nahum , Behar Ehud , Brotherton Michael S. , Chelouche Doron , De Rosa Gisella , Dalla Bontà Elena , Dehghanian Maryam , Ferland Gary J. , Fian Carina , Homayouni Yasaman , Ilić Dragana , Kaspi Shai , Kovačević Andjelka B. , Landt Hermine , Č. Popović Luka , Storchi-Bergmann Thaisa , Wang Jian-Min , Zaidouni Fatima
Published: November 2024

The local (z = 0.0315) active galactic nucleus (AGN) Mrk 817 was monitored over more than 500 days with space-borne and ground-based instruments as part of a large international campaign, AGN STORM 2. Here, we present a comprehensive analysis of the broadband continuum variations using detailed modeling of the broad line region (BLR), several types of disk winds classified by their optical depth, and new numerical simulations. We find that diffuse continuum (DC) emission, with additional contributions from strong and broad emission lines, can explain the continuum lags observed in this source during high- and low-luminosity phases. Disk illumination by the variable X-ray corona contributes only a small fraction of the observed continuum lags. Our BLR models assume radiation-pressure-confined clouds distributed over a distance of 2–122 light days. We present calculated mean emissivity radii of many emission lines, and DC emission, and suggest a simple, transfer-function-dependent method that ties them to cross-correlation lag determinations. We do not find clear indications for large-optical-depth winds, but identify the signature of lower-column-density winds. In particular, we associate the shortest observed continuum lags with a combination of τ(1 Ryd) ≈ 2 wind and a partly shielded BLR. Even smaller optical depth winds may be associated with X-ray absorption features and with noticeable variations in the widths and lags of several high-ionization lines like He ii and C iv. Finally, we demonstrate the effect of torus dust emission on the observed lags in the i and z bands.
Anisotropic Magnetized Asteroseismic Waves
Authors: Tripathi B. , Mitra Dhrubaditya
Published: November 2024

We solve for waves in a polytropic, stratified plasma with a spatially varying background magnetic field that points along the horizontal x-direction, and with gravity that is directed along the vertical z-direction. Force balance determines the magnitude of the background magnetic field,

B

0

2

∼

z

n
+
1

, where n is the polytropic index. Using numerical and asymptotic methods, we deduce an explicit dispersion relation for fast pressure-driven waves:

Ω
2

∼
K

2
m
+
n

[
1
+

1
/

M
A

2

(
4
−
2
γ

+

cos

2

θ
−
3

cos

4

θ
)

/

4
]

. Here, Ω is the frequency, K is the wavenumber, θ is the angle the wavevector makes with the background magnetic field, M
A is the Alfvénic Mach number, and m is an integer representing the eigenstate. We discuss the roles of such an explicit formula in asteroseismology.
Long-term Study of the 2020 Magnetar-like Outburst of the Young Pulsar PSR J1846-0258 in Kes 75
Authors: Sathyaprakash R. , Rea N. , Coti Zelati F. , Borghese A. , Pilia M. , Trudu M. , Burgay M. , Turolla R. , Zane S. , Esposito P. , Mereghetti S. , Campana S. , Götz D. , Ibrahim A. Y. , Israel G. L. , Possenti A. , Tiengo A.
Published: November 2024

Magnetar-like activity has been observed in a large variety of neutron stars. PSR J1846−0258 is a young 327 ms radio-quiet pulsar with a large rotational power (∼8 × 1036 erg s−1), and resides at the center of the supernova remnant Kes 75. It is one of the rare examples of a high-magnetic-field pulsar showing characteristics both of magnetars and radio pulsars, and can thus provide important clues on the differences in the emission mechanisms between these two classes. In 2006, PSR J1846−0258 was detected to undergo an outburst for the first time, accompanied by a large flux increase, millisecond X-ray bursts, significant spectral changes, and a large timing glitch. In the period between 2020 May and June, after 14 yr of quiescent stable emission, the source underwent a second magnetar-like outburst, which was followed up with several observations by Neutron Star Interior Composition Explorer, XMM-Newton, NuSTAR, and Swift. In this work, we report on the long-term timing and X-ray spectral properties of the source following the 2020 outburst, and place upper limits on any source activity at radio wavelengths. We demonstrate that the pulsed flux increased by a factor >6 during the outburst, followed by nontrivial variability in the spin-down rate. Our timing analysis shows that the spin frequency and its derivative are clearly affected by magnetospheric activity due to the outburst. We find hints for an oscillation in the frequency derivative with a timescale of 50–60 days, recovering later on to stable quiescence.
Forecasting the Population of Globular Cluster Streams in Milky Way–type Galaxies
Authors: Pearson Sarah , Bonaca Ana , Chen Yingtian , Gnedin Oleg Y.
Published: November 2024

Thin stellar streams originating from globular clusters (GCs) are among the most sensitive tracers of low-mass dark matter subhalos. Joint analysis of the entire population of stellar streams will place the most robust constraints on the dark matter subhalo mass function, and therefore the nature of dark matter. Here we use a hierarchical model of GC formation to forecast the total number, masses, and radial distribution of dissolved GC in Milky Way–like galaxies. Furthermore, we generate mock stellar streams from these progenitors’ orbital histories taking into account the clusters’ formation and accretion times, mass, and metallicity. Out of ∼10,000 clusters more massive than 104
M
⊙, ∼9000 dissolved in the central bulge and are fully phase mixed at the present, while the remaining ∼1000 survive as coherent stellar streams. This suggests that the current census of ∼80 GC streams in the Milky Way is severely incomplete. Beyond 15 kpc from the Galactic center we are missing ∼100 streams, of which the vast majority are from accreted GCs. Deep Rubin photometry (g ≲ 27.5) would be able to detect these streams, even the most distant ones beyond >75 kpc. We also find that M31 will have an abundance of streams at galactocentric radii of 30–100 kpc. We conclude that future surveys will find a multitude of stellar streams from GCs, which can be used for dark matter subhalo searches.
Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Chen Kan , Dong Ruobing
Published: November 2024

Planet–disk interactions can produce kinematic signatures in protoplanetary disks. While recent observations have detected non-Keplerian gas motions in disks, their origins are still being debated. To explore this, we conduct 3D hydrodynamic simulations using the code FARGO3D to study nonaxisymmetric kinematic perturbations at two scale heights induced by Jovian planets in protoplanetary disks, followed by examinations of detectable signals in synthetic CO emission line observations at millimeter wavelengths. We advocate for using residual velocity or channel maps, generated by subtracting an azimuthally averaged background of the disk, to identify planet-induced kinematic perturbations. We investigate the effects of two basic simulation parameters, simulation duration and numerical resolution, on the simulation results. Our findings suggest that a short simulation (e.g., 100 orbits) is insufficient to establish a steady velocity pattern given our chosen viscosity (α = 10−3) and displays plenty of fluctuations on an orbital timescale. Such transient features could be detected in observations. By contrast, a long simulation (e.g., 1000 orbits) is required to reach steady state in kinematic structures. At 1000 orbits, the strongest detectable velocity structures are found in the spiral wakes close to the planet. Through numerical convergence tests, we find hydrodynamics results converge in spiral regions at a resolution of 14 cells per disk scale height or higher. Meanwhile, synthetic observations produced from hydrodynamic simulations at different resolutions are indistinguishable with 0.″1 angular resolution and 10 hr of integration time on Atacama Large Millimeter/submillimeter Array.
Origin and Full Characterization of the Secondary (Assembly) Halo Bias
Authors: Salvador-Solé Eduard , Manrique Alberto , Agulló Eduard
Published: November 2024

The clustering of dark matter halos depends not only on their mass, the so-called primary bias, but also on their internal properties, the so-called secondary bias. While the former effect is well understood within the Press–Schechter and excursion set models of structure formation, the latter is not. In those models, protohalos are fully characterized by their height and scale, which determine the halo mass and collapse time, so there is no room for any other halo property. This is why the secondary bias was believed not to be innate but due to the distinct merger rate of halos lying in different backgrounds, and dubbed assembly bias. However, it has now been determined that mergers leave no imprint in the inner halo properties. In fact, the innate origin of the secondary bias cannot be discarded because, in the more realistic peak model of structure formation, halo seeds are characterized by one additional property: the peak curvature. Here, we use the confluent system of peak trajectory formalism to show that peaks lying in different backgrounds have different mean curvatures, which in turn cause them to evolve into halos with different typical inner properties. The dependence we find of the properties on halo background (or halo clustering) reproduces the results of simulations.
New Results on the Onset of a Coronal Mass Ejection from 5303 Å Emission Line Observations with VELC/ADITYA-L1
Authors: Ramesh R. , Muthu Priyal V. , Singh Jagdev , Sasikumar Raja K. , Savarimuthu P. , Gavshinde Priya
Published: November 2024

We report on the onset of a coronal mass ejection (CME) using spectroscopic observations in the 5303 Å coronal emission line with the Visible Emission Line Coronagraph (VELC) onboard ADITYA-L1, the recently launched first Indian space solar mission. The CME was observed on 2024 July 16 in association with an X1.9 class soft X-ray flare from heliographic location S05W85. The VELC observations were near the west limb of the Sun during the CME. The results obtained helped to constrain the onset time of the CME. In addition, they indicate a ≈50% decrease in the coronal intensity near the source region of the CME due to mass depletion, a ≈15% enhancement in the emission line width, and a redshifted Doppler velocity of about ≈10 km s−1. The nonthermal velocity associated with the line broadening is ≈24.87 km s−1.
Bolometric Corrections for FU Ori Object Accretion Disk Luminosities
Authors: Carvalho Adolfo S. , Hillenbrand Lynne A.
Published: November 2024

The accretion luminosity of an FU Ori disk is a fundamental system parameter, but a challenging one to estimate for all but the most well-studied systems. FU Ori objects are dynamically evolving accretion disks, especially close in time to the outburst epoch. They have a complex multitemperature disk structure that results in distinctly shaped, broad spectral energy distributions (SEDs). Detailed spectroscopic analysis is required for simultaneous constraint on relevant physical parameters such as the central stellar mass, inner disk radius, disk inclination, and disk accretion rate. However, outbursting systems that are deeply embedded and/or distant may be limited to only photometric measurement and over only a narrow range of wavelengths. The bolometric corrections necessary to estimate accretion luminosities are not straightforward and in particular cannot be adopted from existing literature on isotropically radiating stars. We present bolometric corrections specific to astrophysical accretion disks for a variety of filters in ongoing and upcoming all-sky surveys.
Statistical Analysis of Near-surface Structure and Material Properties on Momentum Transfer in Rubble Pile Targets Impacted by Kinetic Impactors
Authors: DeCoster Mallory E. , Stickle Angela M. , Rainey Emma S. G. , Graninger Dawn M.
Published: November 2024

Rubble pile asteroids consist of reassembled fragments of once larger monolithic asteroid parent bodies. Recent spacecraft missions to asteroids like Itokawa, Ryugu, Bennu, and Dimorphos suggest that rubble pile asteroids are common in the asteroid population, and rubble piles could be a likely structure among potentially hazardous objects. Therefore, it is important to understand the response of rubble pile targets to kinetic impacts for potential future deflection needs. The recent Double Asteroid Redirection Test (DART) mission motivates an investigation of kinetic impacts into rubble pile targets to understand their effects on deflection. Here, we simulate kinetic impacts into Dimorphos-sized asteroid targets to understand the effect of the impact site structure on the deflection efficiency of relevant sizes for planetary defense. We perform 52 two-dimensional simulations where we vary the impact site structure of the impact site, the target porosity, and the material behavior/strength model to understand their relative effects on crater size and the momentum enhancement factor (β). We find that the effects of the impact site on both crater size and β are greatest for impacts into weaker targets, where impact sites rich in matrix material result in statistically larger craters and higher βs compared to impact sites rich in boulder material. Further, impact site structures that promote increased boulder ejection result in larger β values. These results provide important intuition to understand the DART impact and to extrapolate results to future potential missions.
Numerical Investigation of the Cohesive Strength Regime of the Bilobated Arrokoth after the Sky-crater-forming Impact Event
Authors: Kim Yaeji , Hirabayashi Masatoshi , Bauer James
Published: November 2024

In 2019, NASA’s New Horizons mission, using the Long Range Reconnaissance Imager, revealed Arrokoth’s bilobated shape and a large impact-crater-like region (“Sky”) on the small lobe, which is ∼7 km wide and ∼1 km deep. Given that this depression takes up ∼7% of the entire volume of the small lobe, Arrokoth’s neck, the most structurally sensitive area to failure, might have been subject to substantial structural modification if the Sky-crater-forming event occurred after the bilobate shape had formed. Using the π-scaling law, we quantified the linear momentum imparted to the small lobe by the Sky-crater-forming event, which was in the range of (2.4–4.0) × 1013 kg m s−1, depending on Arrokoth’s bulk density of 250–500 kg m−3 and impact speeds of 100 m s−1, 300 m s−1, and 1 km s−1. If the linear momentum was fully transferred to Arrokoth’s small lobe, it would have given the small lobe an impulse velocity of approximately 0.1 m s−1 relative to the large lobe. To assess the structural impact of this event, we used a finite-element modeling approach to simulate post-impact stress fields driven by the estimated impulse velocity on the small lobe and constrained the critical cohesive strength required to prevent structural failure. Based on the current parameter space, our results suggest that the Sky-crater-forming event could have required the critical cohesive strength of up to ∼20 kPa for Arrokoth’s neck to avoid structural failure, which is higher than the typical cohesive strength estimated for small bodies (usually less than 1 kPa for asteroids and comets).
A mathematical model of flavescence dorée in grapevines by considering seasonality
Authors: Huancas Fernando , Coronel Aníbal , Vidal Rodolfo , Berres Stefan , Brito Humberto
Published: November 2024

This paper presents a mathematical model to describe the spread of flavescence dorée, a disease caused by the bacterium Candidatus Phytoplasma vitis, which is transmitted by the insect vector Scaphoideus titanus in grapevine crops. The key contribution of this work is the derivation of conditions under which positive periodic solutions exist. These conditions are based on the assumption that key factors such as recruitment rates, disease transmission, and vector infectivity vary periodically, thus reflecting seasonal changes. The existence of these periodic solutions is proven using the degree theory, and numerical examples are provided to support the theoretical findings. This model aims to enhance the understanding of the epidemiological dynamics of flavescence dorée and contribute to developing better control strategies to manage the disease in grapevines.