Look What I Am Doing: Does Observational Learning Take Place in Evocative Task-Sharing Situations?

Two experiments were conducted to investigate whether physical and observational practice in task-sharing entail comparable implicit motor learning. To this end, the social-transfer-of-learning (SToL) effect was assessed when both participants performed the joint practice task (Experiment 1 \u2013 complete task-sharing), or when one participant observed the other performing half of the practice task (Experiment 2 \u2013 evocative task-sharing). Since the inversion of the spatial relations between responding agent and stimulus position has been shown to prevent SToL, in the present study we assessed it in both complete and evocative task-sharing conditions either when spatial relations were kept constant or changed from the practice to the transfer session. The same pattern of results was found for both complete and evocative task-sharing, thus suggesting that implicit motor learning in evocative task-sharing is equivalent to that obtained in complete task-sharing. We conclude that this motor learning originates from the simulation of the complementary (rather than the imitative) action

Happiness in Italy: Translation, Factorial Structure and Norming of the Subjective Happiness Scale in a Large Community Sample

Abstract The Subjective Happiness Scale (SHS) is one of the most commonly used measures of happiness. Many translations and validation studies have been carried out in different countries and languages. The aim of the current paper was to investigate the psychometric properties of the Italian translation of the SHS and to provide normative data. The SHS was administered with life satisfaction items, anxiety and depression scales to a community sample of 993 participants, aged 18-85 years, living in different parts of Italy. Age and gender distributions were stratified according to the population pyramid. Confirmatory Factor Analysis supported the unidimensionality of the SHS, with acceptable fit indexes (NNFI = .96; CFI = .99; RMSEA = .08; 95 % C.I. [.04-.12]). Multi-group analyses supported total invariance of the SHS measurement model for males and females, and partial invariance for younger (i.e., 18-44 years old) and older (i.e., 45-85 years old) participants. Significant correlations with satisfaction items, anxiety and depression provided evidence for concurrent validity. These findings showed that the Italian SHS translation is a reliable and valid tool, which adds to existing translations and validation studies in different countries and languages

Psychological adjustment and heart rate variability in ovarian cancer survivors

Introduction: Body image, posttraumatic growth, quality of life, coping, and social support are relevant concepts to ovarian cancer survivors. This study aimed to examine the associations among these concepts as well as their relationships with heart rate variability (HRV), which is an index of vagal tone. Methods: an exploratory and correlational study was conducted on 25 ovarian cancer survivors. We used self-report measures to assess psychological variables. HRV parameters recorded for this study were analyzed in the time domain and in the frequency domain. Spearman correlations were performed. Results: Positive attitude coping strategy was associated with psychological and physical distress related to problems of appearance (Rho = -.57, p < .01), emotional functioning (Rho = .53, p < .01), and global health (Rho = .47, p < .05). Problem solving coping strategy was correlated with a higher posttraumatic growth, namely greater personal strength (Rho = .44, p < .05) and better relationships with others (Rho = .40, p < .05). Seeking social support was associated with growth in relationships with others (Rho = .40, p < .05). Higher HRV parameters were associated with higher physical functioning (SDNN: Rho = .59, p < .01; RMSSD: Rho = .54; p < .01; pNN50: Rho = .56, p < .01; HF: Rho = .58, p < .01). The ratio of low-frequency to high-frequency power (LF/HF) was negatively associated with posttraumatic growth (i.e., personal strength: Rho = .51, p < .05; new possibilities: Rho = -.54, p < .01). Discussion: Positive attitude and problem solving coping strategies may facilitate psychological adjustment to ovarian cancer. The strong association between markers of vagal tone and physical functioning offers insights on the possible role of vagus nerve in ovarian cancer survivors. These findings should be further investigated by future studies with larger samples and longitudinal designs

MIDIS: JWST/MIRI reveals the Stellar Structure of ALMA-selected Galaxies in the Hubble-UDF at Cosmic Noon

We present deep James Webb Space Telescope (JWST)/MIRI F560W observations of a flux-limited, ALMA-selected sample of 28 galaxies at z=0.5-3.6 in the Hubble Ultra Deep Field (HUDF). The data from the MIRI Deep Imaging Survey (MIDIS) reveal the stellar structure of the HUDF galaxies at rest-wavelengths of >1 micron for the first time. We revise the stellar mass estimates using new JWST photometry and find good agreement with pre-JWST analysis; the few discrepancies can be explained by blending issues in the earlier lower-resolution Spitzer data. At z~2.5, the resolved rest-frame near-infrared (1.6 micron) structure of the galaxies is significantly more smooth and centrally concentrated than seen by HST at rest-frame 450 nm (F160W), with effective radii of Re(F560W)=1-5 kpc and S\'ersic indices mostly close to an exponential (disk-like) profile (n~1), up to n~5 (excluding AGN). We find an average size ratio of Re(F560W)/Re(F160W)~0.7 that decreases with stellar mass. The stellar structure of the ALMA-selected galaxies is indistinguishable from a HUDF reference sample of galaxies with comparable MIRI flux density. We supplement our analysis with custom-made, position-dependent, empirical PSF models for the F560W observations. The results imply that an older and smoother stellar structure is in place in massive gas-rich, star-forming galaxies at Cosmic Noon, despite a more clumpy rest-frame optical appearance, placing additional constraints on galaxy formation simulations. As a next step, matched-resolution, resolved ALMA observations will be crucial to further link the mass- and light-weighted galaxy structures to the dusty interstellar medium.Comment: 19 pages, 10 figures, 1 table, submitted to Ap

MIDIS. JWST NIRCam and MIRI unveil the stellar population properties of Lyα\alpha-emitters and Lyman-Break galaxies at z ~ 3-7

We study the stellar population properties of 182 spectroscopically-confirmed (MUSE/VLT) Lyman-$\alpha$ emitters (LAEs) and 450 photometrically-selected Lyman-Break galaxies (LBGs) at z = 2.8 - 6.7 in the Hubble eXtreme Deep Field (XDF). Leveraging the combined power of HST and JWST NIRCam and MIRI observations, we analyse their rest-frame UV-through-near-IR spectral energy distributions (SEDs) with MIRI playing a crucial role in robustly assessing the LAE's stellar mass and ages. Our LAEs are low-mass objects (log$_{10}$(M$_\star$[M$_\odot$]) ~ 7.5), with little or no dust extinction (E(B - V) ~ 0.1) and a blue UV continuum slope ($\beta$ ~ -2.2). While 75% of our LAEs are young (< 100 Myr), the remaining 25% have significantly older stellar populations (> 100 Myr). These old LAEs are statistically more massive, less extinct and have lower specific star formation rate (sSFR) compared to young LAEs. Besides, they populate the M$_\star$ - SFR plane along the main-sequence (MS) of star-forming galaxies, while young LAEs populate the starburst region. The comparison between the LAEs properties to those of a stellar-mass matched sample of LBGs shows no statistical difference between these objects, except for the LBGs redder UV continuum slope and marginally larger E(B - V) values. Interestingly, 48% of the LBGs have ages < 10 Myr and are classified as starbursts, but lack detectable Ly$\alpha$ emission. This is likely due to HI resonant scattering and/or selective dust extinction. Overall, we find that JWST observations are crucial in determining the properties of LAEs and shedding light on the properties and similarities between LAEs and LBGs.Comment: 19 pages, 15 figures, 5 tables. Submitted to AP

Life beyond 30: Probing the-20 < M (UV) <-17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey

We present the ultraviolet luminosity function and an estimate of the cosmic star formation rate density at 8 8 galaxy candidates based on their dropout nature in the F115W and/or F150W filters, a high probability for their photometric redshifts, estimated with three different codes, being at z > 8, good fits based on χ 2 calculations, and predominant solutions compared to z < 8 alternatives. We find mild evolution in the luminosity function from z ∼ 13 to z ∼ 8, i.e., only a small increase in the average number density of ∼0.2 dex, while the faint-end slope and absolute magnitude of the knee remain approximately constant, with values α = − 2.2 ± 0.1, and M * = − 20.8 ± 0.2 mag. Comparing our results with the predictions of state-of-the-art galaxy evolution models, we find two main results: (1) a slower increase with time in the cosmic star formation rate density compared to a steeper rise predicted by models; (2) nearly a factor of 10 higher star formation activity concentrated in scales around 2 kpc in galaxies with stellar masses ∼108 M ⊙ during the first 350 Myr of the universe, z ∼ 12, with models matching better the luminosity density observational estimations ∼150 Myr later, by z ∼ 9

Life beyond 30: Probing the −20 < M UV < −17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey

We present the ultraviolet luminosity function and an estimate of the cosmic star formation rate density at 8 8 galaxy candidates based on their dropout nature in the F115W and/or F150W filters, a high probability for their photometric redshifts, estimated with three different codes, being at z > 8, good fits based on χ2 calculations, and predominant solutions compared to z < 8 alternatives. We find mild evolution in the luminosity function from z ∼ 13 to z ∼ 8, i.e., only a small increase in the average number density of ∼0.2 dex, while the faint-end slope and absolute magnitude of the knee remain approximately constant, with values α = − 2.2 ± 0.1, and M* = − 20.8 ± 0.2 mag. Comparing our results with the predictions of state-of-the-art galaxy evolution models, we find two main results: (1) a slower increase with time in the cosmic star formation rate density compared to a steeper rise predicted by models; (2) nearly a factor of 10 higher star formation activity concentrated in scales around 2 kpc in galaxies with stellar masses ∼108M⊙ during the first 350 Myr of the universe, z ∼ 12, with models matching better the luminosity density observational estimations ∼150 Myr later, by z ∼ 9

data set for positivity article

<p>Data set used for a study titled "Does Positivity Mediate the Relation of Extraversion and Neuroticism with Subjective Happiness?"</p