Introduction
Though BDSM interest (bondage & discipline, dominance & submission and sadism & masochism) has proven to be quite prevalent (46.8% in recent research), there is still significant stigma ...surrounding it, both in general society and among mental health practitioners.
Objectives
This research explores the biological mechanisms associated with a BDSM interaction in the hope to strengthen the argument that it does not belong in the psychiatric field.
Methods
The present study collected data on peripheral hormone levels, pain thresholds and pain cognitions before and after a BDSM interaction and compared these results to a control group.
Results
show that submissives have increased cortisol and endocannabinoid levels due to the BDSM interaction and that these increases are linked. Dominants showed a significant increase in endocannabinoids associated with power play but not with pain play. BDSM practitioners have a higher pain threshold overall and a BSDM interaction will result in a temporary elevation of pain thresholds for submissives. Additionally, pain thresholds in dominants will be dependent upon their fear of pain and tendency to catastrophize pain and submissives will experience less fear of pain than the control group
Conclusions
Even though this is one of the first studies of its kind, several biological processes can be associated with BDSM interactions, strengthening the hypothesis of BDSM as a healthy form of intimacy and promoting its distinction from paraphilias as they are described in the DSM or ICD classifications.
Disclosure
No significant relationships.
We make publicly available a catalog of calibrated environmental measures for galaxies in the five 3D-Hubble Space Telescope (HST)/CANDELS deep fields. Leveraging the spectroscopic and grism ...redshifts from the 3D-HST survey, multiwavelength photometry from CANDELS, and wider field public data for edge corrections, we derive densities in fixed apertures to characterize the environment of galaxies brighter than mag in the redshift range . By linking observed galaxies to a mock sample, selected to reproduce the 3D-HST sample selection and redshift accuracy, each 3D-HST galaxy is assigned a probability density function of the host halo mass, and a probability that it is a central or a satellite galaxy. The same procedure is applied to a z = 0 sample selected from Sloan Digital Sky Survey. We compute the fraction of passive central and satellite galaxies as a function of stellar and halo mass, and redshift, and then derive the fraction of galaxies that were quenched by environment specific processes. Using the mock sample, we estimate that the timescale for satellite quenching is it is longer at lower stellar mass or lower redshift, but remarkably independent of halo mass. This indicates that, in the range of environments commonly found within the 3D-HST sample ( ), satellites are quenched by exhaustion of their gas reservoir in the absence of cosmological accretion. We find that the quenching times can be separated into a delay phase, during which satellite galaxies behave similarly to centrals at fixed stellar mass, and a phase where the star formation rate drops rapidly ( Gyr), as shown previously at z = 0. We conclude that this scenario requires satellite galaxies to retain a large reservoir of multi-phase gas upon accretion, even at high redshift, and that this gas sustains star formation for the long quenching times observed.
We present the completed KMOS3D survey, an integral field spectroscopic survey of 739 \(\mathrm{log}({M}_{\star }/{M}_{\odot })\gt 9\) galaxies at 0.6 < z < 2.7 using the K-band Multi Object ...Spectrograph (KMOS) at the Very Large Telescope. The KMOS3D survey provides a population-wide census of kinematics, star formation, outflows, and nebular gas conditions both on and off the star-forming galaxy main sequence through the spatially resolved and integrated properties of Hα, N ii, and S ii emission lines. We detect Hα emission for 91% of galaxies on the main sequence of star formation and 79% overall. The depth of the survey has allowed us to detect galaxies with star formation rates below 1 M ⊙ yr−1, as well as to resolve 81% of detected galaxies with ≥3 resolution elements along the kinematic major axis. The detection fraction of Hα is a strong function of both color and offset from the main sequence, with the detected and nondetected samples exhibiting different spectral energy distribution shapes. Comparison of Hα and UV+IR star formation rates reveal that dust attenuation corrections may be underestimated by 0.5 dex at the highest masses (\(\mathrm{log}({M}_{\star }/{M}_{\odot })\gt 10.5\)). We confirm our first year results of a high rotation-dominated fraction (monotonic velocity gradient and v rot/\({\sigma }_{0}\gt \sqrt{3.36}\)) of 77% for the full KMOS3D sample. The rotation-dominated fraction is a function of both stellar mass and redshift, with the strongest evolution measured over the redshift range of the survey for galaxies with \(\mathrm{log}({M}_{\star }/{M}_{\odot })\lt 10.5\). With this paper, we include a final data release of all 739 observed objects (http://www.mpe.mpg.de/ir/KMOS3D).
In this paper, we follow up on our previous detection of nuclear ionized outflows in the most massive (log(M sub(*)/M sub(middot in circle)) > or =, slanted 10.9) z ~ 1-3 star-forming galaxies by ...increasing the sample size by a factor of six (to 44 galaxies above log(M sub(*)/M sub(middot in circle)) > or =, slanted 10.9) from a combination of the SINS/zC-SINF, LUCI, GNIRS, and KMOS super(3D) spectroscopic surveys. We find a fairly sharp onset of the incidence of broad nuclear emission (FWHM in the Halpha, NII, and SII lines ~450-5300 km s super(-1)), with large NII/Halpha ratios, above log(M sub(*)/M sub(middot in circle)) ~ 10.9, with about two-thirds of the galaxies in this mass range exhibiting this component. Broad nuclear components near and above the Schechter mass are similarly prevalent above and below the main sequence of star-forming galaxies, and at z ~ 1 and ~2. The line ratios of the nuclear component are fit by excitation from active galactic nuclei (AGNs), or by a combination of shocks and photoionization. The incidence of the most massive galaxies with broad nuclear components is at least as large as that of AGNs identified by X-ray, optical, infrared, or radio indicators. The mass loading of the nuclear outflows is near unity. Our findings provide compelling evidence for powerful, high-duty cycle, AGN-driven outflows near the Schechter mass, and acting across the peak of cosmic galaxy formation.
ABSTRACT We measure C iii 1907, C iii 1909 emission lines in 11 gravitationally lensed star-forming galaxies at z ∼ 1.6-3, finding much lower equivalent widths than previously reported for fainter ...lensed galaxies. While it is not yet clear what causes some galaxies to be strong C iii emitters, C iii emission is not a universal property of distant star-forming galaxies. We also examine C iii emission in 46 star-forming galaxies in the local universe, using archival spectra from GHRS, FOS, and STIS on HST and IUE. Twenty percent of these local galaxies show strong C iii emission, with equivalent widths < −5 . Three nearby galaxies show C iii emission equivalent widths as large as the most extreme emitters yet observed in the distant universe; all three are Wolf-Rayet galaxies. At all redshifts, strong C iii emission may pick out low-metallicity galaxies experiencing intense bursts of star formation. Such local C iii emitters may shed light on the conditions of star formation in certain extreme high-redshift galaxies.
For lensed galaxy SGAS J111020.0+645950.8 at redshift z = 2.481, which is magnified by a factor of 28 8, we analyze the morphology of star formation, as traced by rest-frame ultraviolet emission, in ...both the highly magnified source plane and simulations of how this galaxy would appear without lensing magnification. Were this galaxy not lensed, but rather drawn from a Hubble Space Telescope deep field, we would conclude that almost all its star formation arises from an exponential disk (Sérsic index of 1.0 0.4) with an effective radius of measured from two-dimensional fitting to F606W using Galfit, and measured by fitting a radial profile to F606W elliptical isophotes. At the normal spatial resolution of the deep fields, there is no sign of clumpy star formation within SGAS J111020.0+645950.8. However, the enhanced spatial resolution enabled by gravitational lensing tells a very different story; much of the star formation arises in two dozen clumps with sizes of r = 30-50 pc spread across the 7 kpc length of the galaxy. The color and spatial distribution of the diffuse component suggests that still-smaller clumps are unresolved. Despite this clumpy, messy morphology, the radial profile is still well-characterized by an exponential profile. In this lensed galaxy, stars are forming in complexes with sizes well below 100 pc; such sizes are wholly unexplored by surveys of galaxy evolution at .
We stack the rest-frame ultraviolet spectra of N = 14 highly magnified gravitationally lensed galaxies at redshifts . The resulting new composite spans , with a peak signal-to-noise ratio (S/N) of ...103 per spectral resolution element (∼100 km s−1). It is the highest S/N, highest spectral resolution composite spectrum of z ∼ 2-3 galaxies yet published. The composite reveals numerous weak nebular emission lines and stellar photospheric absorption lines that can serve as new physical diagnostics, particularly at high redshift with the James Webb Space Telescope (JWST). We report equivalent widths to aid in proposing for and interpreting JWST spectra. We examine the velocity profiles of strong absorption features in the composite, and in a matched composite of COS/HST galaxy spectra. We find remarkable similarity in the velocity profiles at and , suggesting that similar physical processes control the outflows across cosmic time. While the maximum outflow velocity depends strongly on ionization potential, the absorption-weighted mean velocity does not. As such, the bulk of the high-ionization absorption traces the low-ionization gas, with an additional blueshifted absorption tail extending to at least −2000 km s−1. We interpret this tail as arising from the stellar wind and photospheres of massive stars. Starburst99 models are able to replicate this high-velocity absorption tail. However, these theoretical models poorly reproduce several of the photospheric absorption features, indicating that improvements are needed to match observational constraints on the massive stellar content of star-forming galaxies at . We publicly release our composite spectra.
We introduce Project MegaSaura: the Magellan Evolution of Galaxies Spectroscopic and Ultraviolet Reference Atlas. MegaSaura comprises medium-resolution, rest-frame ultraviolet spectroscopy of N = 15 ...bright gravitationally lensed galaxies at redshifts of 1.68 < z < 3.6, obtained with the MagE spectrograph on the Magellan telescopes. The spectra cover the observed-frame wavelength range 3200 < λo < 8280 ; the average spectral resolving power is R = 3300. The median spectrum has a signal-to-noise ratio (S/N) = 21 per resolution element at 5000 . As such, the MegaSaura spectra have superior S/N and wavelength coverage compared to what COS/HST provides for starburst galaxies in the local universe. This paper describes the sample, the observations, and the data reduction. We compare the measured redshifts for the stars, the ionized gas as traced by nebular lines, and the neutral gas as traced by absorption lines; we find the expected bulk outflow of the neutral gas, and no systemic offset between the redshifts measured from nebular lines and the redshifts measured from the stellar continuum. We provide the MegaSaura spectra to the astronomical community through a data release.
Introduction
BDSM is an acronym describing bondage & discipline, dominance & submission and sadism & masochism. Afflicting or receiving pain is usually an important part of the BDSM interaction.
...Objectives
This research focuses on better understanding the aspect of pain within a BDSM interaction by investigating the differences in 1) baseline pain thresholds, 2) the impact of a BDSM interaction on those thresholds and 3) threshold moderating factors like pain cognition between submissive and dominant BDSM participants and control individuals.
Methods
Submissive and dominant counterparts of 35 couples were recruited to participate in a BDSM interaction, of which 34 dominants and 33 submissives were included in analyses. A non-BDSM interested control group (n=27) was included to control for social interaction, of which 24 were included in analyses. Pain threshold measurements were measured at three points in time and pain cognitions scales were taken.
Results
BDSM practitioners have a higher pain threshold overall and a BSDM interaction will result in a temporary elevation of pain thresholds for submissives. Additionally, pain thresholds in dominants will be dependent upon their fear of pain and tendency to catastrophize pain and submissives will experience less fear of pain than the control group.
Conclusions
This study helps shed further light on the biological processes behind a BDSM interaction through pain threshold measurements. By enhancing our understanding of the mechanisms behind a BDSM interaction in this way, we aspire to relieve the stigma these practitioners still endure.
Disclosure
No significant relationships.
Introduction
The past years BDSM (an acronym for bondage and discipline, dominance and submission, and sadism and masochism) has gained a significant amount of attention and popularity in the general ...population, portraying an inaccurate image of BDSM and the people who share these interests. Yet despite this increasing popularity, only little empirical research has focused on this subject and it’s possible driving mechanisms so far, sustaining the existing misconceptions and stigma towards BDSM in general and BDSM practitioners in specific.
Objectives
We aimed to gain more insights on understanding the underlying psychological mechanisms, such as sensation seeking and coping, in people who participate in BDSM-related activities, as well as into the factors which contribute to the existing stigma and discrimination
Methods
In a national survey study 256 Dutch-speaking BDSM-practitioners were compared to a matched sample of people from the general Belgian population (N = 300) who lack any interest in BDSM in two separate studies.
Results
About 86% of the general population maintained stigmatizing beliefs about these sexual interests and practices. In regard to sensation seeking and coping, compared to controls, BDSM practitioners reported signifcantly higher levels of sensation seeking for all dimensions, as well as the use of more active coping skills.
Conclusions
People who do not conform to the current social standards of our society often seem to remain the subject of stigmatization and discrimination. Further research is needed to explore the psychological processes that drive BDSM interests in order to destigmatize and normalize consensual BDSM-related activities.
Disclosure
No significant relationships.
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