Visual Extinction Research Articles

A NEW DETERMINATION OF THE BINDING ENERGY OF ATOMIC OXYGEN ON DUST GRAIN SURFACES: EXPERIMENTAL RESULTS AND SIMULATIONS

The energy to desorb atomic oxygen from an interstellar dust grain surface, $E_{\rm des}$, is an important controlling parameter in gas-grain models; its value impacts the temperature range over which oxygen resides on a dust grain. However, no prior measurement has been done of the desorption energy. We report the first direct measurement of $E_{\rm des}$ for atomic oxygen from dust grain analogs. The values of $E_{\rm des}$ are $1660\pm 60$~K and $1850\pm 90$~K for porous amorphous water ice and for a bare amorphous silicate film, respectively, or about twice the value previously adopted in simulations of the chemical evolution of a cloud. We use the new values to study oxygen chemistry as a function of depth in a molecular cloud. For $n=10^4$ cm$^{-3}$ and $G_0$=10$^2$ ($G_0$=1 is the average local interstellar radiation field), the main result of the adoption of the higher oxygen binding energy is that H$_2$O can form on grains at lower visual extinction $A_{\rm V}$, closer to the cloud surface. A higher binding energy of O results in more formation of OH and H$_2$O on grains, which are subsequently desorbed by FUV radiation, with consequences for gas-phase chemistry. For higher values of $n$ and $G_0$, the higher binding energy can lead to a large increase in the column of H$_2$O but a decrease in the column of O$_2$.

Tong Luo Jiu Nao ameliorates Aβ1-40-induced cognitive impairment on adaptive behavior learning by modulating ERK/CaMKII/CREB signaling in the hippocampus.

BackgroundTong Luo Jiu Nao (TLJN), a modern formula of Chinese medicine extracts on the basis of Traditional Chinese Medicine theory, has been used to treat dementia. The present study aimed to investigate its ameliorating effects on Aβ1–40-induced cognitive impairment in rats using a series of novel reward-directed instrumental learning (RDIL) tasks, and to determine its possible mechanism of action.MethodsRats were pretreated with TLJN extract (0.9 and 1.8 g/kg, p.o.) for 10 daysbefore surgery, and were trained to gain reward reinforcement by lever pressing at the meantime. Thereafter, rats received a bilateral microinjection of Aβ1–40 in CA1 regions of the hippocampus. Cognitive performance was evaluated with the goal directed (higher response ratio) and habit (visual signal discrimination and extinction) learning tasks, as well as on the levels of biochemical parameters and molecules.ResultsOur findings first demonstrated that TLJN can improve Aβ1–40-induced amnesia in RDIL via enhancing the comprehension of action-outcome association and the utilization of cue information to guide behavior. Then, its ameliorating effects should attribute to the modulation of ERK/CaMKII/CREB signaling in the hippocampus.ConclusionTLJN can markedly enhance cognitions of Aβ1–40 microinjection animal model in adaptive behavioral tasks. It has the potential, possibly as complementary and alternative therapy, to prevent and/or delay the deterioration of cognitive impairment in AD.

Processing of bilateral versus unilateral conditions: Evidence for the functional contribution of the ventral attention network

Processing of multiple or bilateral conditions presented simultaneously in both hemifields reflects the natural mode of perception in our multi-target environment, but is not yet completely understood. While region-of-interest based studies in healthy subjects reported single cortical areas as the right inferior parietal lobe (IPL) or temporoparietal junction (TPJ) to process bilateral conditions, studies in extinction patients with reduced ability in this regard suggested the right superior temporal cortex to hold a key role. The present fMRI study on healthy subjects aimed at resolving these discrepancies by contrasting bilateral versus unilateral visual conditions in a paradigm similar to the bed-side test for patients with visual extinction on a whole brain level. Additionally, reduced attentional capacity in spatial processing was investigated in normal aging. Processing of bilateral conditions compared to unilateral ones showed to require stronger activation of not one single cortical region but the entire right-lateralized ventral attention network, bilateral parietal and visual association areas. These results might suggest a conceptual difference between unilateral and bilateral spatial processing with the latter depending on additional anatomical and functional brain resources. Reduced attentional capacity in elderly subjects was associated with compensatory recruitment of contralateral functional homologues [left IPL, TPJ, frontal eye field (FEF)]. These data reveal the functional anatomy of our ability to visually process and respond to the entity of the environment and improve our understanding of neglect and extinction. Moreover, the data demonstrate that a restriction of the attentional capacity is based on processing limitations in the network of high-level cortical areas and not due to restriction in the primary sensory ones.

Modelling [C i] emission from turbulent molecular clouds

We use detailed numerical simulations of the coupled chemical, thermal and dynamical evolution of the gas in a turbulent molecular cloud to study the usefulness of the [CI] 609 micron and 370 micron fine structure emission lines as tracers of cloud structure. Emission from these lines is observed throughout molecular clouds, and yet the question of what we can learn from them about the physics of the clouds remains largely unexplored. We show that the fact that [CI] emission is widespread within molecular clouds is a simple consequence of the fact that the clouds are dominated by turbulent motions. Turbulence creates large density inhomogeneities, allowing radiation to penetrate deeply into the clouds. As a result, [CI] emitting gas is found throughout the cloud, rather than being concentrated at the edges. We examine how well we can use [CI] emission to trace the structure of the cloud, and show that the integrated intensity of the 609 micron line traces column density accurately over a wide range of visual extinctions. For extinctions greater than a few, [CI] and 13CO both perform well, but [CI] becomes a superior tracer of column densities for visual extinctions A_V <= 3 We have also studied the distribution of [CI] excitation temperatures in the gas, and show that these are typically smaller than the kinetic temperature, indicating that most of the carbon atoms are not in local thermodynamic equilibrium. We discuss how best to determine T_ex from observations of the [CI] lines, and how to use these values to estimate the column density of neutral atomic carbon. We show that even in the best case, we tend to systematically underestimate the atomic carbon content of the gas. Our results suggest that observationally-derived estimates of the atomic carbon content of real GMCs could be in error by as much as a factor of two.

Modelling grain alignment by radiative torques and hydrogen formation torques in reflection nebula

Reflection nebulae--dense cores--illuminated by surrounding stars offer a unique opportunity to directly test our quantitative model of grain alignment based on radiative torques (RATs) and to explore new effects arising from additional torques. In this paper, we first perform detailed modeling of grain alignment by RATs for the IC 63 reflection nebula illuminated both by a nearby $\gamma$ Cas star and the diffuse interstellar radiation field. We calculate linear polarization $p_{\lambda}$ of background stars by radiatively aligned grains and explore the variation of fractional polarization ($p_{\lambda}/A_V$) with visual extinction $A_{V}$ across the cloud. Our results show that the variation of $p_{V}/A_{V}$ versus $A_{V}$ from the dayside of IC 63 to its center can be represented by a power-law ($p_{V}/A_{V}\propto A_{V}^{\eta}$) with different slopes depending on $A_{V}$. We find a shallow slope $\eta \sim- 0.1$ for $A_{V}< 3$ and a very steep slope $\eta\sim -2$ for $A_{V}> 4$. We then consider the effects of additional torques due to H$_{2}$ formation and model grain alignment by joint action of RATs and H$_2$ torques. We find that $p_{V}/A_{V}$ tends to increase with an increasing magnitude of H$_{2}$ torques. In particular, the theoretical predictions obtained for $p_{V}/A_{V}$ and peak wavelength $\lambda_{\max}$ in this case show an improved agreement with the observational data. Our results reinforce the predictive power of the RAT alignment mechanism in a broad range of environmental conditions and show the effect of pinwheel torques in environments with efficient H$_2$ formation. Physical parameters involved in H$_2$ formation may be constrained using detailed modeling of grain alignment combined with observational data. In addition, we discuss implications of our modeling for interpreting latest observational data by {\it Planck} and other ground-based instruments.

Abstract W MP35: The Re-examining Acute Eligibility for Thrombolysis Task Force Criteria for Defining Rapidly Improving Stroke Symptoms: A Pilot Prospective Study of tPA Treatment Decisions

Background: Rapidly Improving Stroke Symptoms (RISS) is a controversial exclusion criterion for tPA for acute ischemic stroke (AIS). Prior studies suggest 4-44% of AIS patients eligible are not given tPA solely because of RISS and their outcome is not invariably benign. In 2013 The Re-examining Acute Eligibility for Thrombolysis (TREAT) Task Force published new criteria for defining RISS. Objectives: To estimate frequency and outcome of RISS based on TREAT criteria in a prospective cohort of consecutive AIS patients. Methods: Serial NIH Stroke Scales (NIHSS) for AIS patients admitted within 4.5 hrs of symptom onset were performed every 20 (±5) minutes until a treatment decision (tPA vs no tPA) was made, independent of the study. Improvement was calculated as the difference between baseline NIHSS (bNIHSS) and treatment decision NIHSS (tdNIHSS). Per TREAT criteria, RISS was defined as improvement to a non-disabling mild stroke and none of the following deficits present: complete hemianopsia; severe aphasia; visual or sensory extinction; any weakness limiting sustained effort against gravity; any total NIHSS &gt;5; any remaining deficit considered potentially disabling by the patient and the treater. We compared frequency and outcomes of TREAT-based RISS with the most commonly used RISS definition [≥4 point improvement (4PI) on NIHSS]. Good outcome was defined as modified Rankin Scale of 0-1 at 3 months. Results: Fifty AIS were enrolled: mean age 65 yrs; median bNIHSS=5 (IQR 2,11); median tdNIHSS=5 (IQR 2,9); tPA was given in 23 (46%). Five/50 (10%) were RISS according to TREAT criteria, all 5 had good outcome at 90 days without tPA. Five/50 (10%) were RISS according to 4PI, and only 2/5 (40%) had good outcome while 1/5 (20%) died. Conclusions: This is the first preliminary, prospective estimate of RISS frequency and outcome according to TREAT criteria vs. a commonly used RISS definition. Our pilot data suggest the TREAT RISS frequency is in the lower end of prior retrospective estimates and, as a more restrictive definition, may better predict good outcome of RISS in future, larger studies.

Formation of dense structures induced by filament collisions

Context. The Pipe nebula is a molecular cloud that lacks star formation feedback and has a relatively simple morphology and velocity structure. This makes it an ideal target to test cloud evolution through collisions. Aims. We aim at drawing a comprehensive picture of this relatively simple cloud to better understand the formation and evolution of molecular clouds on large scales. Methods. We use archival data to compare the optical polarization properties, the visual extinction, and the 13CO velocities and linewidths of the entire cloud in order to identify trends among the observables. Results. The Pipe nebula can be roughly divided in two filaments with different orientations and gas velocity ranges: E-W at 2-4 km s-1 and N-S at 6-7 km s-1. The two filaments overlap at the bowl, where the gas shows a velocity gradient spanning from 2 to 7 km s-1. Compared to the rest of the Pipe nebula, the bowl gas appears to be denser and exhibits larger linewidths. In addition, the polarization data at the bowl shows lower angular dispersion and higher polarization degree. Cores in the bowl tend to cluster in space and tend to follow the 13CO velocity gradient. In the stem, cores tend to cluster in regions with properties similar to those of the bowl. Conclusions. The velocity pattern points to a collision between the filaments in the bowl region. The magnetic field seems to be compressed and strengthened in the shocked region. The proportional increase of density and magnetic field strength by a factor similar to the Alfv\'enic Mach number suggests a continuous shock at low Alfv\'enic Mach number under flux-freezing. Shocked regions seem to enhance the formation and clustering of dense cores.

GRAIN ALIGNMENT IN STARLESS CORES

We present near infrared polarimetry data of background stars shining through a selection of starless cores taken in the $K$ band, probing visual extinctions up to $A_{V} \sim 48$. We find that $P_K/{\tau _K}$ continues to decline with increasing $A_{V}$ with a power law slope of roughly -0.5. Examination of published submillimeter (submm) polarimetry of starless cores suggests that by $A_{V} \gtrsim 20$ the slope for $P$ vs. $\tau$ becomes $\sim -1$, indicating no grain alignment at greater optical depths. Combining these two data sets, we find good evidence that, in the absence of a central illuminating source, the dust grains in dense molecular cloud cores with no internal radiation source cease to become aligned with the local magnetic field at optical depths greater than $A_V \sim 20$. A simple model relating the alignment efficiency to the optical depth into the cloud reproduces the observations well.

MAPPING THE INTERSTELLAR MEDIUM WITH NEAR-INFRARED DIFFUSE INTERSTELLAR BANDS

We map the distribution and properties of the Milky Way's interstellar medium as traced by diffuse interstellar bands (DIBs) detected in near-infrared stellar spectra from the SDSS-III/APOGEE survey. Focusing exclusively on the strongest DIB in the H-band, at ~1.527 microns, we present a projected map of the DIB absorption field in the Galactic plane, using a set of about 60,000 sightlines that reach up to 15 kpc from the Sun and probe up to 30 magnitudes of visual extinction. The strength of this DIB is linearly correlated with dust reddening over three orders of magnitude in both DIB equivalent width (W_DIB) and extinction, with a power law index of 1.01 +/- 0.01, a mean relationship of W_DIB/A_V = 0.1 Angstrom mag^-1, and a dispersion of ~0.05 Angstrom mag^-1 at extinctions characteristic of the Galactic midplane. These properties establish this DIB as a powerful, independent probe of dust extinction over a wide range of A_V values. The subset of about 14,000 robustly detected DIB features have an exponential W_DIB distribution. We empirically determine the intrinsic rest wavelength of this transition to be lambda_0 = 15,272.42 Angstrom, and then calculate absolute radial velocities of the carrier, which display the kinematical signature of the rotating Galactic disk. We probe the DIB carrier distribution in three dimensions and show that it can be characterized by an exponential disk model with a scaleheight of about 100 pc and a scalelength of about 5 kpc. Finally, we show that the DIB distribution also traces large-scale Galactic structures, including the central long bar and the warp of the outer disk.

Star formation around the mid-infrared bubble CN 148

We present a multi-wavelength study to analyse the star formation process associated with the mid-infrared bubble CN 148 (H II region G10.3-0.1), which harbors an O5V-O6V star. The arc-shaped distribution of molecular CO(2-1) emission, the cold dust emission, and the polycyclic aromatic hydrocarbon features trace a photodissociation region (PDR) around the H II region. We have identified 371 young stellar objects (YSOs) in the selected region and, interestingly, their spatial distribution correlates well with the PDR. 41% of these YSOs are present in 13 clusters, each having visual extinction larger than 16 mag. The clusters at the edges of the bubble (both northeast and southwest) are found to be relatively younger than the clusters located further away from the bubble. We also find that four 6.7 GHz methanol masers, two Extended Green Objects, an ultra-compact H II region, and a massive protostar candidate (as previously reported) are spatially positioned at the edges of the bubble. The existence of an apparent age gradient in YSO clusters and different early evolutionary stages of massive star formation around the bubble suggest their origin to be influenced by an H II region expanding into the surrounding interstellar medium. The data sets are suggestive of triggered star formation.

A HIGH-RESOLUTION STUDY OF NEAR-INFRARED DIFFUSE INTERSTELLAR BANDS

We present high-resolution echelle spectroscopic observations of the two near-infrared (NIR) diffuse interstellar bands (DIBs) at 13175 Å and 11797.5 Å. The DIBs have been observed in a number of diffuse interstellar medium sightlines that exhibit a wide range of visual extinctions. Band profiles are similar to those seen in narrow DIBs, clearly asymmetric and can be closely fitted in most cases using two simple Gaussian components. Gaussian fits were generally found to be more successful than fits based on a multiple-cloud model using a template DIB profile. For a sample of nine objects in which both bands are observed, the strength of both NIR DIBs generally increases with A(V), and we report a correlation between the two observed bands over a large A(V) range and widely separated lines of sight. The strength of the two bands is also compared against those of two visual DIBs and the diffuse ISM aliphatic dust absorption feature at 3.4 μm previously detected in the same sightlines. We find that the NIR DIBs do not exhibit notable (anti)correlations with either. Implications of these observations on possible DIB carrier species are discussed.

Once you feel it, you see it: Insula and sensory-motor contribution to visual awareness for fearful bodies in parietal neglect

The interplay between the neural mechanisms of visual awareness and those involved in emotion processing and the mapping of related somatic changes remains unclear. To address this issue we studied one patient with visual extinction following right parietal damage, in a combined behavioral, psychophysiological and neuroimaging experiment. Patient M.P. was presented with neutral and fearful bodily expressions, either unilaterally in the left (LVF) or right visual field (RVF), or in both visual fields simultaneously. Fearful expressions presented in the left visual field simultaneously with neutral bodies in the RVF were detected more often than left-side neutral bodies. Signal detection analysis showed that the preferential access of fearful bodies to visual awareness is related to higher perceptual sensitivity for these stimuli during attentional competition. Pupil dilation, which indexes autonomic arousal, increased for fearful more than for neutral bodies. Moreover, dilation for extinguished fearful bodies was bigger than for consciously perceived fearful bodies. This decoupling between (increased) arousal and (lack of) conscious visual experience argues against a direct relationship between visual awareness of emotional signals and peripheral changes. Neuroimaging results showed that fearful bodies activated the left amygdala and extrastriate cortex when consciously perceived as well as when extinguished. Critically, however, conscious perception of fearful bodies was uniquely associated with activity in the anterior insula, somatosensory, motor and premotor cortex (PMC), and the cerebellum. This suggests that the integration between peripheral arousal and the moment-to-moment mapping at the central neural level of these bodily changes is critical for the conscious visual experience of emotional signals.

SPATIALLY RESOLVED CHEMISTRY IN NEARBY GALAXIES. III. DENSE MOLECULAR GAS IN THE INNER DISK OF THE LIRG IRAS 04296+2923

We present a survey of 3 mm molecular lines in IRAS 04296+2923, one of the brightest known molecular-line emitting galaxies, and one of the closest LIRGs. Data are from the Owens Valley and CARMA millimeter interferometers. Species detected at ~<4" resolution include C^18O, HCN, HCO+, HNC, CN, CH_3OH and, tentatively, HNCO. Along with existing CO, ^13CO and radio continuum data, these lines constrain the chemical properties of the inner disk. Dense molecular gas in the nucleus fuels a star formation rate ~>10 M_sun/yr and is traced by lines of HCN, HCO+, HNC, and CN. A correlation between HCN and star formation rate is observed on sub-kpc scales, consistent with global relations. Toward the nucleus, CN abundances are similar to those of HCN, indicating emission comes from a collection (~40-50) of moderate visual extinction, photon-dominated region clouds. The CO isotopic line ratios are unusual: CO(1-0)/^13CO(1-0) and CO(1-0)/C^18O(1-0) line ratios are large toward the starburst, as is commonly observed in LIRGs, but farther out in the disk these ratios are remarkably low (~<3). ^13CO/C^18O abundance ratios are lower than in Galactic clouds, possibly because the C^18O is enriched by massive star ejecta from the starburst. ^13CO is underabundant relative to CO. Extended emission from CH_3OH indicates that dynamical shocks pervade both the nucleus and the inner disk. The unusual CO isotopologue ratios, the CO/HCN intensity ratio versus L_IR, the HCN/CN abundance ratio and the gas consumption time versus inflow rate, all indicate that the starburst in IRAS 04296+2923 is in an early stage of development.

PHOTON-DOMINATED REGION MODELING OF THE [C I], [C II], AND CO LINE EMISSION FROM A BOUNDARY IN THE TAURUS MOLECULAR CLOUD

We present [Ci] and [Cii] observations of a linear edge region in the Taurus molecular cloud, and model this region as a cylindrically symmetric PDR exposed to a low-intensity UV radiation field. The sharp, long profile of the linear edge makes it an ideal case to test PDR models and determine cloud parameters. We compare observations of the [C i], 3P1 -> 3P0 (492 GHz), [C i] 3P2 -> 3P1 (809 GHz), and [Cii] 2P3/2 -> 2P1/2 (1900 GHz) transitions, as well as the lowest rotational transitions of 12CO and 13CO, with line intensities produced by the RATRAN radiative transfer code from the results of the Meudon PDR code. We constrain the density structure of the cloud by fitting a cylindrical density function to visual extinction data. We study the effects of variation of the FUV field, 12C/13C isotopic abundance ratio, sulfur depletion, cosmic ray ionization rate, and inclination of the filament relative to the sky-plane on the chemical network of the PDR model and resulting line emission. We also consider the role of suprathermal chemistry and density inhomogeneities. We find good agreement between the model and observations, and that the integrated line intensities can be explained by a PDR model with an external FUV field of 0.05 G0, a low ratio of 12C to 13C ~ 43, a highly depleted sulfur abundance (by a factor of at least 50), a cosmic ray ionization rate (3 - 6) x 10-17 s^-1, and without significant effects from inclination, clumping or suprathermal chemistry.

IRAM 30 m LARGE SCALE SURVEY OF12CO(2-1) AND13CO(2-1) EMISSION IN THE ORION MOLECULAR CLOUD

Using the IRAM 30m telescope we have surveyed a $1\times0.8^{\circ}$ part of the Orion molecular cloud in the $^{12}$CO and $^{13}$CO (2-1) lines with a maximal spatial resolution of $\sim$11" and spectral resolution of $\sim$ 0.4 km~s$^{-1}$. The cloud appears filamentary, clumpy and with a complex kinematical structure. We derive an estimated mass of the cloud of 7700 M$_{\text{Sun}}$ (half of which is found in regions with visual extinctions $A_V$ below $\sim$10) and a dynamical age for the nebula of the order of 0.2 Myrs. The energy balance suggests that magnetic fields play an important role in supporting the cloud, at large and small scales. According to our analysis, the turbulent kinetic energy in the molecular gas due to outflows is comparable to turbulent kinetic energy resulting from the interaction of the cloud with the HII region. This latter feedback appears negative, i.e. the triggering of star formation by the HII region is inefficient in Orion. The reduced data as well as additional products such as the column density map are made available online at http://userpages.irap.omp.eu/~oberne/Olivier_Berne/Data.

On the radiation driven alignment of dust grains: Detection of the polarization hole in a starless core

We aim to investigate the polarization properties of a starless core in a very early evolutionary stage. Linear polarization data reveal the properties of the dust grains in the distinct phases of the interstellar medium. Our goal is to investigate how the polarization degree and angle correlate with the cloud and core gas. We use optical, near infrared and submillimeter polarization observations toward the starless object Pipe-109 in the Pipe nebula. Our data cover a physical scale range of 0.08 to 0.4 pc, comprising the dense gas, envelope and the surrounding cloud. The cloud polarization is well traced by the optical data. The near infrared polarization is produced by a mixed population of grains from the core border and the cloud gas. The optical and near infrared polarization toward the cloud reach the maximum possible value and saturate with respect to the visual extinction. The core polarization is predominantly traced by the submillimeter data and have a steep decrease with respect to the visual extinction. Modeling of the submillimeter polarization indicates a magnetic field main direction projected onto the plane-of-sky and loss of grain alignment for densities higher than $6\times10^4$ cm$^{-3}$ (or $A_V > 30$ mag). Pipe-109 is immersed in a magnetized medium, with a very ordered magnetic field. The absence of internal source of radiation significantly affects the polarization efficiencies in the core, creating a polarization hole at the center of the starless core. This result supports the theory of dust grain alignment via radiative torques.

Cingulate neglect in humans: Disruption of contralesional reward learning in right brain damage

Motivational valence plays a key role in orienting spatial attention. Nonetheless, clinical documentation and understanding of motivationally based deficits of spatial orienting in the human is limited. Here in a series of one group-study and two single-case studies, we have examined right brain damaged patients (RBD) with and without left spatial neglect in a spatial reward-learning task, in which the motivational valence of the left contralesional and the right ipsilesional space was contrasted. In each trial two visual boxes were presented, one to the left and one to the right of central fixation. In one session monetary rewards were released more frequently in the box on the left side (75% of trials) whereas in another session they were released more frequently on the right side. In each trial patients were required to: 1) point to each one of the two boxes; 2) choose one of the boxes for obtaining monetary reward; 3) report explicitly the position of reward and whether this position matched or not the original choice. Despite defective spontaneous allocation of attention toward the contralesional space, RBD patients with left spatial neglect showed preserved contralesional reward learning, i.e., comparable to ipsilesional learning and to reward learning displayed by patients without neglect. A notable exception in the group of neglect patients was L.R., who showed no sign of contralesional reward learning in a series of 120 consecutive trials despite being able of reaching learning criterion in only 20 trials in the ipsilesional space. L.R. suffered a cortical-subcortical brain damage affecting the anterior components of the parietal-frontal attentional network and, compared with all other neglect and non-neglect patients, had additional lesion involvement of the medial anterior cingulate cortex (ACC) and of the adjacent sectors of the corpus callosum. In contrast to his lateralized motivational learning deficit, L.R. had no lateral bias in the early phases of attentional processing as he suffered no contralesional visual or auditory extinction on double simultaneous tachistoscopic and dichotic stimulation and detected, with no exception, single contralesional visual and auditory stimuli. In a separate study, we were able to compare L.R. with another RBD patient, G.P., who had a selective lesion in the right ACC, in the adjacent callosal connections and the medial-basal prefrontal cortex. G.P. had no contralesional neglect and displayed normal reward learning both in the left and right side of space. These findings show that contralesional reward learning is generally preserved in RBD patients with left spatial neglect and that this can be exploited in rehabilitation protocols. Contralesional reward learning is severely disrupted in neglect patients when an additional lesion of the ACC is present: however, as demonstrated by the comparison between L.R. and G.P. cases, selective unilateral lesion of the right ACC does not produce motivational neglect for the contralesional space.

DIFFUSE INTERSTELLAR BANDS VERSUS KNOWN ATOMIC AND MOLECULAR SPECIES IN THE INTERSTELLAR MEDIUM OF M82 TOWARD SN 2014J

We discuss the absorption due to various constituents of the interstellar medium of M82 seen in moderately high resolution, high signal-to-noise ratio optical spectra of SN 2014J. Complex absorption from M82 is seen, at velocities 45 $\le$ $v_{\rm LSR}$ $\le$ 260 km s$^{-1}$, for Na I, K I, Ca I, Ca II, CH, CH$^+$, and CN; many of the diffuse interstellar bands (DIBs) are also detected. Comparisons of the column densities of the atomic and molecular species and the equivalent widths of the DIBs reveal both similarities and differences in relative abundances, compared to trends seen in the ISM of our Galaxy and the Magellanic Clouds. Of the ten relatively strong DIBs considered here, six (including $\lambda$5780.5) have strengths within $\pm$20% of the mean values seen in the local Galactic ISM, for comparable N(K I); two are weaker by 20--45% and two (including $\lambda$5797.1) are stronger by 25--40%. Weaker than "expected" DIBs [relative to N(K I), N(Na I), and E(B-V)] in some Galactic sight lines and toward several other extragalactic supernovae appear to be associated with strong CN absorption and/or significant molecular fractions. While the N(CH)/N(K I) and N(CN)/N(CH) ratios seen toward SN 2014J are similar to those found in the local Galactic ISM, the combination of high N(CH$^+$)/N(CH) and high W(5797.1)/W(5780.5) ratios has not been seen elsewhere. The centroids of many of the M82 DIBs are shifted, relative to the envelope of the K I profile -- likely due to component-to-component variations in W(DIB)/N(K I) that may reflect the molecular content of the individual components. We compare estimates for the host galaxy reddening E(B-V) and visual extinction A$_{\rm V}$ derived from the various interstellar species with the values estimated from optical and near-IR photometry of SN 2014J.

Extensive HST ultraviolet spectra and multiwavelength observations of SN 2014J in M82 indicate reddening and circumstellar scattering by typical dust

SN 2014J in M82 is the closest detected Type Ia supernova (SN Ia) in at least 28 years and perhaps in 410 years. Despite its small distance of 3.3 Mpc, SN 2014J is surprisingly faint, peaking at V = 10.6 mag, and assuming a typical SN Ia luminosity, we infer an observed visual extinction of A_V = 2.0 +/- 0.1 mag. But this picture, with R_V = 1.6 +/- 0.2, is too simple to account for all observations. We combine 10 epochs (spanning a month) of HST/STIS ultraviolet through near-infrared spectroscopy with HST/WFC3, KAIT, and FanCam photometry from the optical to the infrared and 9 epochs of high-resolution TRES spectroscopy to investigate the sources of extinction and reddening for SN 2014J. We argue that the wide range of observed properties for SN 2014J is caused by a combination of dust reddening, likely originating in the interstellar medium of M82, and scattering off circumstellar material. For this model, roughly half of the extinction is caused by reddening from typical dust (E(B-V ) = 0.45 mag and R_V = 2.6) and roughly half by scattering off LMC-like dust in the circumstellar environment of SN 2014J.

Contralesional rTMS relieves visual extinction in chronic stroke

Patients affected by right parietal lobe lesion can be severely impaired in sustained attention tasks, particularly in the left visual field. For example, patients with right parietal stroke are commonly limited in their ability to attentionally track multiple moving objects in their left visual field when competing stimuli are simultaneously presented in the right, ipsilesional visual field. This is a hallmark of visual extinction, a failure to respond to contralesional visual stimuli, when competing stimuli are presented in the good hemifield. It has been hypothesized that post-stroke hyperactivity of the undamaged left hemisphere leads to excessive cross-hemispheric inhibition of the damaged right hemisphere, thus exacerbating the attentional deficits. However, there has been no direct physiological demonstration of this hypothesis, as most of the studies are conducted using unilateral tasks, a condition not sufficient to drive inter-hemispheric competition. The inter-hemispheric inhibition hypothesis also raises the possibility that if hyperactivity of the healthy hemisphere were reduced, this could relieve inter-hemispheric inhibition, disinhibiting the damaged hemisphere and potentially restoring some function. To test this hypothesis, and to examine whether we could relieve deficits in sustained attention in right parietal patients, we used repetitive transcranial magnetic stimulation (rTMS) to reduce the activity of the left, healthy hemisphere. Six patients suffering from visual extinction underwent two counterbalanced sessions: low frequency rTMS over the left parietal lobe and sham control stimulation. The patients׳ performance in an attentional tracking task significantly improved in the contralesional visual field immediately after rTMS, but not after sham. Performance remained unaltered in the ipsilesional field. We hypothesize that rTMS temporarily releases the damaged right hemisphere from excessive cross-hemispheric inhibition by the hyperactive healthy hemisphere, leading to some cognitive recovery after cortical lesion.