Impact of High School Preparation on College Oral Communication Apprehension

This study examines the impact of high school public speaking skills training and public speaking experiences on college overall communication apprehension (CA) and public speaking context CA. The results show that public speaking skill-training in high school is significantly related to lower CA levels or students upon entering a college-level basic speech course. In addition, students who report more public speaking experiences both in high school setting and outside the high school setting, tend to report lower overall CA and lower CA in the public speaking context

Communication Apprehension and Basic Course Success: The Lab-supported Public Speaking Course Intervention

This study examined a lab-supported public speaking course as an intervention for helping reduce overall and context communication apprehension (CA) for high and moderate CA students. In addition, this study queried whether actual lab usage was related to CA reduction and to course grade for those students. Results showed that the lab-supported public speaking course helped high and moderate CAs significantly reduce overall CA and CA in public speaking, group discussions, meetings and interpersonal conversation contexts. There was no difference in reduction of CA level between high and moderate CAs who utilized the speech lab and those who did not. However, high CAs who utilized the speech lab earned higher course grades than those who did not use the lab

Connected Classroom Climate and Communication in the Basic Course: Associations with Learning

Most research on the association between classroom climate and student learning has emphasized the instructor’s role in creating a positive learning environment. However, the role students play in fostering a classroom climate that promotes learning has received less attention, particularly in the basic course. This study examined the relationship between perceptions of a connected classroom climate and students’ cognitive and affective learning involving 437 freshman and sophomore university students enrolled in the basic public speaking course. Students completed the Connected Classroom Climate Inventory (CCCI) and scales measuring affective and cognitive learning. Results showed significant relationships between student perceptions of connected classroom climate and cognitive learning, affective learning, and affective behavioral intent

”Musta se on vaa kiva, että se ylipäätään tulee sinne luokkaan”:opettajien ja oppilaiden käsityksiä koira-avusteisesta pedagogiikasta

Tiivistelmä. Tämän pro gradu -tutkielman tavoitteena on tarkastella koulukoiratoiminnan toteutusta sekä oppilaiden ja opettajien käsityksiä koulukoiratoiminnasta eräässä pohjoissuomalaisessa yhtenäiskoulussa. Tutkielman teoreettisessa viitekehyksessä esitellään eläinavusteisen ja koira-avusteisen toiminnan muotoja ja vaikutuksia sekä koiran roolia ja merkitystä kasvatustyössä aiemman tutkimuskirjallisuuden perusteella. Tutkimus toteutettiin fenomenografisena tapaustutkimuksena. Aineisto kerättiin tutkimuskoulun oppilailta, opettajilta ja koulukoiran ohjaajana toimivalta oppilashuollon työntekijältä teemahaastattelujen avulla. Haastatteluja toteutettiin yhteensä kymmenen, joista neljä oli oppilaiden ryhmähaastatteluja. Aineisto analysoitiin aineistolähtöisellä sisällönanalyysillä. Tutkimustulosten perusteella voidaan todeta, että sekä opettajien että oppilaiden käsitykset koulukoirasta ovat hyvin positiivisia ja koulukoira on saanut koululla myönteisen vastaanoton. Koulukoiran nähtiin parantavan oppilaan henkistä hyvinvointia, lisäävän iloa ja mielekkyyttä koulunkäyntiin, vahvistavan lapsen tunne- ja vuorovaikutustaitoja ja vähentävän häiriökäyttäytymistä. Opettajien mukaan koira luo hyväksyvää ja lämmintä tunnelmaa, mikä helpottaa vaikeistakin asioista puhumista ja siten tukee lapsen ja aikuisen välisen keskusteluyhteyden syntymistä. Koiran myös nähtiin tukevan tuntityöskentelyä, lisäävän motivaatiota sekä helpottavan erityisesti ääneen lukemista. Toisaalta erityisesti oppilaat kokivat koiran läsnäolon ja siitä johtuvan innostuksen myös jossain määrin heikentävän työrauhaa ja keskittymistä tuntitilanteissa. Tutkimuksen tulokset olivat suurimmalta osin linjassa aiemman tutkimustiedon kanssa. Tulosten perusteella voidaan päätellä, että koulukoiratoiminnan avulla on mahdollista tukea monipuolisesti oppilaan oppimista ja koulunkäyntiä sekä psyykkistä ja sosiaalista hyvinvointia. Lisäksi koulukoiran läsnäolo voi tutkimustulosten perusteella parantaa myös opettajan työhyvinvointia

The host galaxy and late-time evolution of the Super-Luminous Supernova PTF12dam

Super-luminous supernovae of type Ic have a tendency to occur in faint host galaxies which are likely to have low mass and low metallicity. PTF12dam is one of the closest and best studied super-luminous explosions that has a broad and slowly fading lightcurve similar to SN 2007bi. Here we present new photometry and spectroscopy for PTF12dam from 200-500 days (rest-frame) after peak and a detailed analysis of the host galaxy (SDSS J142446.21+461348.6 at z = 0.107). Using deep templates and image subtraction we show that the full lightcurve can be fit with a magnetar model if escape of high-energy gamma rays is taken into account. The full bolometric lightcurve from -53 to +399 days (with respect to peak) cannot be fit satisfactorily with the pair-instability models. An alternative model of interaction with a dense CSM produces a good fit to the data although this requires a very large mass (~ 13 M_sun) of hydrogen free CSM. The host galaxy is a compact dwarf (physical size ~ 1.9 kpc) and with M_g = -19.33 +/- 0.10, it is the brightest nearby SLSN Ic host discovered so far. The host is a low mass system (2.8 x 10^8 M_sun) with a star-formation rate (5.0 M_sun/year), which implies a very high specific star-formation rate (17.9 Gyr^-1). The remarkably strong nebular lines provide detections of the [O III] \lambda 4363 and [O II] \lambda\lambda 7320,7330 auroral lines and an accurate oxygen abundance of 12 + log(O/H) = 8.05 +/- 0.09. We show here that they are at the extreme end of the metallicity distribution of dwarf galaxies and propose that low metallicity is a requirement to produce these rare and peculiar supernovae.Comment: 20 pages, 12 figures, 8 tables, accepted for publication to MNRA

The multi-faceted Type II-L supernova 2014G from pre-maximum to nebular phase

We present multi-band ultraviolet, optical, and near-infrared photometry, along with visual-wavelength spectroscopy, of supernova (SN) 2014G in the nearby galaxy NGC 3448 (25 Mpc). The early-phase spectra show strong emission lines of the high ionisation species He II/N IV/C IV during the first 2-3 d after explosion, traces of a metal-rich CSM probably due to pre-explosion mass loss events. These disappear by day 9 and the spectral evolution then continues matching that of normal Type II SNe. The post-maximum light curve declines at a rate typical of Type II-L class. The extensive photometric coverage tracks the drop from the photospheric stage and constrains the radioactive tail, with a steeper decline rate than that expected from the $^{56}$Co decay if $\gamma$-rays are fully trapped by the ejecta. We report the appearance of an unusual feature on the blue-side of H$\alpha$ after 100 d, which evolves to appear as a flat spectral feature linking H$\alpha$ and the O I doublet. This may be due to interaction of the ejecta with a strongly asymmetric, and possibly bipolar CSM. Finally, we report two deep spectra at ~190 and 340 d after explosion, the latter being arguably one of the latest spectra for a Type II-L SN. By modelling the spectral region around the Ca II, we find a supersolar Ni/Fe production. The strength of the O I $\lambda\lambda$6300,6363 doublet, compared with synthetic nebular spectra, suggests a progenitor with a zero-age main-sequence mass between 15 and 19 M$_\odot$.Comment: 24 pages, 14 figure

SNhunt151: An explosive event inside a dense cocoon

Indexación: Scopus.We thank S. Spiro, R. Rekola, A. Harutyunyan, and M. L. Graham for their help with the observations. We are grateful to the collaboration of Massimo Conti, Giacomo Guerrini, Paolo Rosi, and Luz Marina Tinjaca Ramirez from the Osservatorio Astronomico Provinciale di Montarrenti. The staffs at the different observatories provided excellent assistance with the observations.The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 267251, ‘Astronomy Fellowships in Italy’ (AstroFIt)’. NE-R acknowledges financial support from MIUR PRIN 2010-2011, ‘The Dark Universe and the Cosmic Evolution of Baryons: From Current Surveys to Euclid’. NE-R, AP, SB, LT, MT, and GP are partially supported by the PRIN-INAF 2014 (project ‘Transient Universe: Unveiling New Types of Stellar Explosions with PESSTO’). GP acknowledges support provided by the Millennium Institute of Astrophysics (MAS) through grant IC120009 of the Programa Iniciativa Cientíifica Milenio del Ministerio de Economía, Fomento y Turismo de Chile. TK acknowledges financial support from the Emil Aaltonen Foundation. CRTS was supported by the NSF grants AST-0909182, AST-1313422, and AST-1413600. AVF is grateful for generous financial assistance from the Christopher R. Redlich Fund, the TABASGO Foundation, the Miller Institute for Basic Research in Science (UC Berkeley), and NASA/HST grant GO-14668 from the Space Telescope Science Institute, which is operated by AURA, Inc. under NASA contract NAS5-26555. The work of AVF was conducted in part at the Aspen Center for Physics, which is supported by NSF grantPHY-1607611; he thanks the Center for its hospitality during the neutron stars workshop in June and July 2017. NE-R acknowledges the hospitality of the ‘Institut de Ciències de l'Espai (CSIC), where this work was completed.This research is based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofísica de Canarias; the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma; the Italian Telescopio Nazionale Galileo (TNG), operated on the island of La Palma by the Fundaci Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias; the Liverpool Telescope, operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias with financial support from the UK Science and Technology Facilities Council; the 1.82-m Copernico Telescope and the Schmidt 67/92 cm of INAF-Asiago Observatory; the Catalina Real Time Survey (CRTS) Catalina Sky Survey (CSS) 0.7-m Schmidt Telescope; and the Las Cumbres Observatory (LCO) network. This work is also based in part on archival data obtained with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS5-26555; the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA (support was provided by NASA through an award issued by JPL/Caltech); and the Swift telescope.This work has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.SNhunt151 was initially classified as a supernova (SN) impostor (nonterminal outburst of a massive star). It exhibited a slow increase in luminosity, lasting about 450 d, followed by a major brightening that reaches M V ≈ -18 mag. No source is detected to M V ≳ -13 mag in archival images at the position of SNhunt151 before the slow rise. Low-to-mid-resolution optical spectra obtained during the pronounced brightening show very little evolution, being dominated at all times by multicomponent Balmer emission lines, a signature of interaction between the material ejected in the new outburst and the pre-existing circumstellar medium. We also analysed mid-infrared images from the Spitzer Space Telescope, detecting a source at the transient position in 2014 and 2015. Overall, SNhunt151 is spectroscopically a Type IIn SN, somewhat similar to SN 2009ip. However, there are also some differences, such as a slow pre-discovery rise, a relatively broad light-curve peak showing a longer rise time (~50 d), and a slower decline, along with a negligible change in the temperature around the peak (T ≤ 10 4 K). We suggest that SNhunt151 is the result of an outburst, or an SN explosion, within a dense circumstellar nebula, similar to those embedding some luminous blue variables like η Carinae and originating from past mass-loss events. © 2017 The Author(s).https://academic.oup.com/mnras/article/475/2/2614/479530

Connected Classroom Climate and Communication Apprehension: Correlations and Implications of the Basic Course

Although scholars have recommended increasing relational variables in the classroom such as familiarity, acquaintance level, and collaboration to help students moderate communication apprehension (CA), few, if any, academic studies have investigated the relationship between CA and a supportive climate among students in the college classroom. Self-report data were collected from 523 undergraduate students from a Midwestern university who participated in a large curriculum assessment program using the Connected Classroom Climate Inventory (CCCI) and the PRCA-24. Results showed significant relationships between student perceptions of connected-classroom climate and CA levels throughout the course

AT 2017be - a new member of the class of Intermediate-Luminosity Red Transients

We report the results of our spectrophotometric monitoring campaign for AT~2017be in NGC~2537. Its lightcurve reveals a fast rise to an optical maximum, followed by a plateau lasting about 30 days, and finally a fast decline. Its absolute peak magnitude ($M_{r}$ $\simeq$ $-$12 $\rm{mag}$) is fainter than that of core-collapse supernovae, and is consistent with those of supernova impostors and other Intermediate-Luminosity Optical Transients. The quasi-bolometric lightcurve peaks at $\sim$ 2 $\times$ 10$^{40}$ erg s$^{-1}$, and the late-time photometry allows us to constrain an ejected $^{56}$Ni mass of $\sim$ 8 $\times$ 10$^{-4}$\msun. The spectra of AT~2017be show minor evolution over the observational period, a relatively blue continuum showing at early phases, which becomes redder with time. A prominent H$\alpha$ emission line always dominates over other Balmer lines. Weak Fe {\sc ii} features, Ca~{\sc ii} H$\&$K and the Ca {\sc ii} NIR triplet are also visible, while P-Cygni absorption troughs are found in a high resolution spectrum. In addition, the [Ca~{\sc ii}] $\lambda$7291,7324 doublet is visible in all spectra. This feature is typical of Intermediate-Luminosity Red Transients (ILRTs), similar to SN~2008S. The relatively shallow archival Spitzer data are not particularly constraining. On the other hand, a non-detection in deeper near-infrared HST images disfavours a massive Luminous Blue Variable eruption as the origin for AT~2017be. As has been suggested for other ILRTs, we propose that AT~2017be is a candidate for a weak electron-capture supernova explosion of a super-asymptotic giant branch star, still embedded in a thick dusty envelope.Comment: 21 pages, 15 figures, accepted by MNRA

Leveraging remotely sensed non-wall-to-wall data for wall-to-wall upscaling in forest inventory

Remote sensing (RS) has enhanced forest inventory with model-based inference, that is, a family of statistical procedures rigorously estimates the parameter of a variable of interest (VOI) for a spatial population, e.g., the mean or total of forest carbon for a study area. Upscaling in earth observation, alias to this estimation, aggregates VOI from a finer spatial resolution to a coarser one with reduced uncertainty, serving decision making for natural resource management at larger scales. However, conventional model-based estimation (CMB) confronts a major challenge: it only supports RS wall-to-wall data, meaning that remotely sensed data must be available in panorama and non-wall-to-wall but quality data such as lidar or even cloud-masked satellite imagery are not supported due to incomplete coverage, impeding precise upscaling with cutting-edge instruments or for large scale applications. Consequently, this study aims to develop and demonstrate the use and usefulness of RS nonwall-to-wall data for upscaling with Hierarchical model-based estimation (HMB) which incorporates a two-stage model for bridging RS non- and wall-to-wall data; and for optimizing cost-efficiency, to evaluate the effects of non-wall-to-wall sample size on upscaling precision. Three main conclusions are relevant: (1) the HMB is a variant of the CMB estimator through trading in the uncertainty of the second-stage model to enable estimation using RS non-wall-to-wall data; (2) a quality first-stage model is key to exerting the advantage of HMB relative to the CMB estimator; (3) the variance of the HMB estimator is dominated by the first-stage model variance component, indicating that increasing the sample size in the first-stage is effective for increasing the overall precision. Overall, the HMB estimator balances tradeoffs between cost, efficiency and flexibility when devising a model-based upscaling in earth observation