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Mushrooms are consumed worldwide because of their nutritional, medicinal values as well as pleasant taste and flavour. Wild edible mushrooms are source of livelihood for poor and landless people which they consume and sell the surplus mushrooms in the nearby market. Many people are not aware about the edibility of wild mushrooms which are generally confined to the tribal areas. However, tribals are aware of the edible mushrooms due to their age-old traditional uses and fond of hunting mushrooms during rainy season. The present paper deals with availability, collection, consumption pattern of wild edible mushrooms by tribals communities, along with preservation and economical contribution of Termitomyces heimii, a popular wild edible mushrooms profusely growing during rainy season of the Similipal, state of Odisha, India. Similipal has a greater diversity of mushrooms throughout the length and breadth due to its varying soil and climate conditions. T. heimii collected the tribal people from near forest area in 4-5 different times in huge quantities during July to October. It partly consumed and rest of the mushroom are sold in the market at a price of Rupees 300/- to 400/-. Termitomyces were more frequently available in Sal (Shorea robusta) forests. Many traders visit forest fringe villages and collect this mushroom from local collector’s and sell it in the marker with profit. Due to its taste, the mushroom has got very high demand in this locality that, it is sold within 5-6 hours after reaching to market. It is assessed that mushrooms worth 14 lakhs are sold in Baripada alone a nearly town of Similipal. The valuation T. heimii alone made by the authors during the field assessment showed that, the entire of Similipal is contributing economically nearly 1.2 crore value of mushrooms as contribution towards livelihood of tribal people. In interior areas tribal people preserve the mushrooms after drying it and consume later during after the season is end. During the study, a survey was conducted in villages adjoining to the forests and local markets to assess the quantities of mushrooms collected from forest and the value of selling valve on the market. Exercise was conducted to know the traditional preservation practice of this mushroom by tribals. From the present investigation, it is concluded that T. heimii is an important wild edible mushroom from Similipal which provides, nutrition and economic boost to the tribals in Similipal region. This promising species can be explored for its domestication in view of its preferred food value as well as a livelihood support of the rural poor people.

COVID-19 is arguably the biggest health crisis the world has faced in the 21st century. Therefore, two of the polyherbal formulations, Infuza and Kulzam were assessed for the prevention of COVID-19 infection as a repurposed medication. Four hundred seven high-risk subjects were recruited in the present open-label randomized controlled clinical trial for eligibility. After assessment for eligibility, remaining 251 subjects were randomized to the test and control groups. Further, 52 high-risk subjects in Infuza, 51 in Kulzam, 51 in InfuzaKulzam and 53 in control group completed the 14 days of intervention/assessment. The phenotyping of lymphocytes at baseline (0 day) and after 14 days of treatment was carried out by flow cytometry assays. A total of 15.09% high-risk subjects in control group turned positive as compared to only 7.69% in Infuza, 3.92% in Kulzam and 1.96% in InfuzaKulzam groups. The rate of conversion to COVID-19 infection in InfuzaKulzam group was minimal and statistically significant as compared to control group (p0.017). No significant changes in phenotype of lymphocytes (T, B, NK cells), absolute lymphocyte count and cytokine levels were found in study groups. However, there was a decreasing trend of hs-CRP level in high-risk subjects after intervention of polyherbal formulations for 14 days. The combination of Infuza and Kulzam may synergistically prevent COVID-19 infection in high-risk subjects of COVID-19.

Background:Sthoulyais a disorder dominated bymedadhatudue to abnormal accumulation of meda in Gatra pradeshaspecifically in Sphik, Udara, Stanaand Gala. It is caused by morbid kapha doshainitially and later pitta and Vaatainvolved in its pathogenesis. This vitiated Dosha or Doshas afflict. The medadhatuinvolving medovaha srotasproduces the related symptom of its own srotas. Further in later stage due abnormal accumulation of Abadha apachita medain other respective srotasexhibits lakshanas like Javoparodha, Ayusohrasa, and Swedabadhaetc. as its complication. The mode of onset is usually gradual depending upon the Nidana‟slike Atisampurna aahara, Avyaayama, Manasika bhava‟s, Beejadoshajaand by Nidanarthakara karana‟s.The involvement of pitta and vaata dosha‟s along kapha doshain the pathogenesis of Sthoulya can be well appreciated by their symptoms like Swedadhikya, Atikshudha, Ati Pipasa, Dourgandhya, Javoparodha, Dourbalya, and Utshahanietc Aim:To assess the clinical efficacy of Vidangadi churna and Amrutadya guggulin the management of Sthoulya(obesity). Materials and Methods:The clinical studies were conducted by the Randomized Comparative Clinical Study method; this method compared the clinical efficacy of Vidangadi churna and Amrutadya guggulin the management of Sthoulya(obesity). Result:In Group A, 2 patients (10%) were shown marked improvement, 16 patients (80%) were shown moderate improvement and 2 patients (10%) were shown mild improvement. In Group B, 3 patients (15%) were shown marked improvement, 15 patients ( 75% ) were shown moderate improvement and 2 patients (10% ) were shown mild improvement. Conclusion-There is no much difference in the results of the both the treatment. Both the drug significantly effective.

We present stellar variability towards the young open cluster NGC\,6823. Time series $V$- and $I$-band CCD photometry led to identification and characterization of 88 variable stars, of which only 14 have been previously recognized. We ascertain the membership of each variable with optical $UBVI$ and infrared photometry, and with Gaia EDR3 parallax and proper motion data. Seventy two variable stars are found to be cluster members, of which 25 are main sequence stars and 48 are pre-main-sequence stars. The probable cluster members collectively suggest an isochrone age of the cluster to be about 2~Myrs based on the GAIA photometry. With the color and magnitude, as well as the shape of the light curve, we have classified the main sequence variables into $\beta$~Cep, $\delta$~Scuti, slowly pulsating B type, and new class variables. Among the pre-main-sequence variables, eight are classical T Tauri variables, and four are Herbig Ae/Be objects, whereas the remaining belong to the weak-lined T Tauri population. The variable nature of 32 stars is validated with TESS light curves. Our work provides refined classification of variability of pre-main-sequence and main-sequence cluster members of the active star-forming complex, Sharpless\,86. Despite no strong evidence of the disk-locking mechanism in the present sample of TTSs, one TTS with larger $\Delta(I-K)$ is found to be slow rotator., Comment: 19 pages, 19 figures, accepted for publication in MNRAS

The infants admitted in the Neonatal Intensive Care Unit (NICU) always need a Hygienic environment and round the clock observations. Infants or the just born babies always express their physical and emotional needs through cry. Thus, the detection of the reasons behind the infant cry plays a vital role in monitoring the health of the babies in the NICU. In this paper, we have proposed a novel approach for detecting the reasons for Infant's cry. In the proposed approach the cry signal of the infant is captured and from this signal, the unique set of features are extracted using MFCCs, LPCCs, and Pitch. This set of features is used to differentiates the patters signals to recognize the reasons for the cry. The reasons for cry such as hunger, pain, sleep, and discomfort are used to represent different classes. The Neural Network Multilayer classifier is designed to recognize the reasons for the cry using the standard dataset of infant cry. The proposed classifier can achieve accuracy of 93.24% from the combined features of MFCCs, LPCCs and Pitch using

We attempted a comprehensive site response study of Garhwal-Kumaun Himalaya in the Central seismic Gap (CSG) using the data collected from 97 strong motion, microtremor and broadband stations. Site...

We report the analysis of high temporal resolution ground and space based photometric observations of SZ Lyncis, a binary star one of whose components is a high amplitude $\delta$ Scuti. UBVR photometric observations were obtained from Mt. Abu Infrared Observatory and Fairborn Observatory; archival observations from the WASP project were also included. Furthermore, the continuous, high quality light curve from the TESS project was extensively used for the analysis. The well resolved light curve from TESS reveals the presence of 23 frequencies with four independent modes, 13 harmonics of the main pulsation frequency of 8.296943$\pm$0.000002 d$^{-1}$ and their combinations. The frequency 8.296 d$^{-1}$ is identified as the fundamental radial mode by amplitude ratio method and using the estimated pulsation constant. The frequencies 14.535 d$^{-1}$, 32.620 d$^{-1}$ and 4.584 d$^{-1}$ are newly discovered for SZ Lyn. Out of these three, 14.535 d$^{-1}$ and 32.620 d$^{-1}$ are identified as non-radial lower order p-modes and 4.584 d$^{-1}$ could be an indication of a g-mode in a $\delta$ Scuti star. As a result of frequency determination and mode identification, the physical parameters of SZ Lyn were revised by optimizations of stellar pulsation models with the observed frequencies. The theoretical models correspond to 7500 K $\le $T$_{\rm eff}$ $\le$ 7800 K, log(g)=3.81$\pm$0.06. The mass of SZ Lyn was estimated to be close to 1.7--2.0 M$_\odot$ using evolutionary sequences. The period-density relation estimates a mean density $\rho$ of 0.1054$\pm$0.0016 g cm$^{-3}$, Comment: 16 pages, 11 figures, accepted for publication in MNRAS

For the B-type supergiant κ Cassiopeiae (HD 2905), variabilities with periods between several hours and a few days have been observed both photometrically and spectroscopically. A recent study of this star by Simón-Díaz et al. has revealed variability with a dominant period of 2.7 d. To understand this variability, we present a linear non-adiabatic stability analysis with respect to radial perturbations for models of κ Cassiopeiae. Instabilities associated with the fundamental mode and the first overtone are identified for models with masses between 27 and 44 M⊙. For selected models, the instabilities are followed into the nonlinear regime by numerical simulations. As a result, finite amplitude pulsations with periods between 3 and 1.8 d are found. The model with a mass of 34.5 M⊙ exhibits a pulsation period of 2.7 d consistent with the observations. In the nonlinear regime, the instabilities may cause a substantial inflation of the envelope.

We present a study based on the high-resolution spectroscopy and K2 space photometry of five chemically peculiar stars in the region of the open cluster M44. The analysis of the high-precision photometric K2 data reveals that the light variations in HD 73045 and HD 76310 are rotational in nature and caused by spots or cloud-like co-rotating structures, which are non-stationary and short-lived. The time-resolved radial velocity measurements, in combination with the K2 photometry, confirm that HD 73045 does not show any periodic variability on timescales shorter than 1.3 d, contrary to previous reports in the literature. In addition to these new rotational variables, we discovered a new heartbeat system, HD 73619, where no pulsational signatures are seen. The spectroscopic and spectropolarimetric analyses indicate that HD 73619 belongs to the peculiar Am class, with either a weak or no magnetic field considering the 200 G detection limit of our study. The Least-Squares Deconvolution (LSD) profiles for HD 76310 indicate a complex structure in its spectra suggesting that this star is either part of a binary system or surrounded by a cloud shell. When placed in the Hertzsprung-Russell diagram, all studied stars are evolved from main-sequence and situated in the $\delta$ Scuti instability strip. The present work is relevant for further detailed studies of CP stars, such as inhomogeneities (including spots) in the absence of magnetic fields and the origin of the pulsational variability in heartbeat systems., Comment: Accepted for publication in MNRAS

Diabetes mellitus is associated with increased levels of inflammation and oxidative stress in patients. The aim of the present study was to test the hypothesis that aqueous extract of Cichorium intybus seeds (AECIS) would have add-on beneficial effect in type 2 diabetes mellitus (T2DM). In this double-blind randomized clinical study, 150 subjects were enrolled to assess the add-on efficacy and safety of AECIS in T2DM patients. The subjects were randomized (1:1) to the AECIS (n = 51) and placebo (n = 49) groups. The subjects in both groups continued to take prescribed doses of metformin. The standardization of AECIS was carried out by liquid chromatography-mass spectrometry and phytochemical analysis. The mean hemoglobin A1c (HbA1c) level in the AECIS and placebo groups at baseline was 8.6% and 8.5%, respectively. Mean values of HbA1c at the end of 12 weeks of intervention were 7.42% in the AECIS group (a reduction of 1.18% from baseline) and 8.4% in the placebo group (mean reduction of 0.1% from baseline). Besides, significant reduction in inflammation, oxidative stress, and hypertriglyceridemia was seen in the AECIS group (p < .05). The study shows for the first time that AECIS supplementation ameliorates the disease progression and it is beneficial as a potential adjunct dietary supplement for the management of T2DM.

We present a comprehensive photometric analysis of a young open cluster NGC 1960 (M36) along with the long-term variability study of this cluster. Based on the kinematic data of Gaia DR2, the membership probabilities of 3871 stars are ascertained in the cluster field among which 262 stars are found to be cluster members. Considering the kinematic and trigonometric measurements of the cluster members, we estimate a mean cluster parallax of 0.86+/-0.05 mas and mean proper motions of mu_RA = -0.143+/-0.008 mas/yr, mu_Dec = -3.395+/-0.008 mas/yr. We obtain basic parameters of the cluster such as E(B-V) = 0.24+/-0.02 mag, log(Age/yr)=7.44+/-0.02, and distance = 1.17+/-0.06 kpc. The mass function slope in the cluster for the stars in the mass range of 0.72-7.32 M_solar is found to be ��= -1.26+/-0.19. We find that mass segregation is still taking place in the cluster which is yet to be dynamically relaxed. This work also presents first high-precision variability survey in the central 13'x13' among which 72 are periodic variables. Among them, 59 are short-period (P1 day). The variable stars have V magnitudes ranging between 9.1 to 19.4 mag and periods between 41 minutes to 10.74 days. On the basis of their locations in the H-R diagram, periods and characteristic light curves, the 20 periodic variables belong to the cluster. We classified them as 2 delta-Scuti, 3 gamma-Dor, 2 slowly pulsating B stars, 5 rotational variables, 2 non-pulsating B stars and 6 as miscellaneous variables., Accepted for publication on December 20, 2019 in MNRAS. 20 pages, 15 figures, 12 tables

We present the results of the high-resolution (R$\sim$60,000) spectroscopic analysis of the star LAMOSTJ045019.27+394758.7 (hereafter J045) from the list of carbon stars of LAMOST DR2. From our analysis, we find that J045 does not exhibit the spectral characteristics of carbon stars. It is found to be a metal-poor ( [Fe/H] = $-$1.05) giant that shows very unusual elemental abundances, particularly for N, Na, V, and Zn. J045 shows ${\alpha}$-elements (Mg, Si, Ca) with near-solar values ($$ = 0.09) in contrast to Galactic stars that show [$\alpha$/Fe] in the range 0.2 to 0.3 dex. In J045, Sc and Ti are under abundant with [X/Fe] $\le$ $-$0.25. Vanadium gives [V/Fe] = 0.51 and zinc is under-abundant with [Zn/Fe] = $-$0.62. The object exhibits near-solar abundances for Sr, Y, Ba, Pr, and Sm. The La is marginally enhanced, and Ce and Nd are marginally under-abundant in J045. With [Ba/Eu] = $-$0.38, the object falls into the category of neutron-capture rich r-I stars. The estimated abundances of various elements show that the observed abundance pattern is not compatible with the abundances characteristic of Galactic metal-poor stars but matches quite closely with the abundance pattern of Sculptor Dwarf galaxy stars of similar metallicity. Based on the above observational evidences, we suggest that the object is a possible Sculptor Dwarf Galaxy escapee., Comment: Accepted for publication in MNRAS

Cysticercosis is considered a common healthcare problem, especially in developing countries. The invasion of muscle by the larval stage of the pork tapeworm, Taenia solium (i.e., Cysticercus cellulosae) usually occurs in association with CNS cysts, concurrent muscle cysts, or both. Isolated skeletal muscle involvement is rare and presents with nonspecific symptoms resulting in a diagnostic dilemma for the treating physician. We report a 20-year-old female with isolated cysticercosis of right sternocleidomastoid muscle presenting as a right neck swelling and mild pain for 4 months, whose diagnosis was established by ultrasonography (USG) and computed tomogram (CT) scan. She was managed conservatively with oral albendazole therapy for four weeks resulting in complete resolution.

Introduction: The traumatic or internal derangement of the knee requires certain investigations for the establishment of diagnosis. With advances in technology and because of high resolution and accuracy a MRI scan is now a standard for evaluating the knee injuries before a subsequent arthroscopy. When used properly after a thorough clinical examination, an MRI can prove to be an efficient and non-invasive diagnostic tool in the management of knee injuries. On the other hand, arthroscopy is considered as the gold standard method for the diagnosis of such injuries. Methods: The prospective hospital based study was conducted on fifty one symptomatic patients with knee injuries over a period of one year. All the patients underwent MRI of the knee joint on Philips Achieva 1.5 Tesla MRI Machine in Bir Hospital, NAMS and they were evaluated and cross checked by faculty members. After proper evaluation, diagnostic arthroscopy was done, if needed therapeutic intervention was also performed. The sensitivity, the specificity, the positive predictive value and the negative predictive value of MRI for MM, LM, ACL and PCL were calculated. Results: A total of 51 patients were included with a mean age of 30.92 years. Left knee was predominantly involved in 56.1% of the cases with 43.9% involvement of right knee. Overall, MRI showed a total of 32 medial menisci tears and 8 lateral menisci tears. There were 5 false negative cases for MMT. MRI revealed tears of ACL in 44 patients and no patient with PCL tear. Arthroscopy revealed ACL tears in 44 cases and confirmed no patient with PCL tear. Conclusions: MRI is a noninvasive, useful and reliable diagnostic tool for evaluating knee injury and it can be used as a first line of investigation in patients with knee injury.

The nominal Kepler mission provided very high-precision photometric data. Using these data, interesting phenomena such as spots, and ``hump and spike'' features were observed in the light curves of some normal A and metallic lined A stars (Am stars). However, the connection between such phenomena and the chemical peculiarity of the Am stars is still unclear. In order to make progress on these issues, its important to collect high-resolution spectroscopic data to determine their fundamental parameters and individual chemical abundances. In this paper, we present a spectroscopic study of a sample of ``hump and spike'' stars in the nominal Kepler field. We used data collected with the High Efficiency and Resolution Mercator \'{E}chelle Spectrograph (HERMES). We determined the spectral type of these stars and obtained the atmospheric stellar parameters such as effective temperatures, surface gravities, projected rotational, microturbulent and radial velocities. We also performed a detailed individual chemical abundance analysis for each target. We confirmed KIC 3459226 and KIC 6266219 as Am stars, KIC 9349245 as a marginal Am star, while KIC 4567097, KIC 4818496, KIC 5524045, KIC 5650229, KIC 7667560, and KIC 9272082 are non-Am stars. To estimate their evolutionary phases, all the stars were placed in the Hertzsprung-Russell (HR) diagram. Based on their spectral classification and chemical abundance pattern, we reclassified KIC 6266219 (previously treated as chemically normal) as an Am star (kA3hA7mF1) and KIC 9272082 (previously treated as Am) as non-Am., Comment: 17 pages, 9 figures, accepted for publication in MNRAS

Microchannels are one of the most significant parts for the Lab-on-Chip applications. The microchannels fabrication is a crucial task. The Soft Lithography is one of the most favored methods of microchannel fabrication. The use of CO2 LASER machining for microchannel fabrication using Acrylic sheet is studied in this paper. The experimentation is carried out to see the effect of LASER scanning speed and laser power on the depth of the microchannel mold. It has observed that the channel depth is increasing linearly with increasing LASER power and decreasing with increase in speed. The straight microchannel configuration with Y shaped inlet having circular & elliptical obstacles has been fabricated using CO2 laser machining on acrylic sheet. Also, the fabricated molds are used to prepare the further microchannel molds using the Soft Lithography technique and then the microchannels prepared from Soft Lithography are used as a mold for the lab-on-chip applications like check the mixing length & mixing phenomenon etc.

We present here optical I-band photometric variability study down to $\simeq$ 19 mag of a young ($\sim$2-3 Myr) star-forming region IC 348 in the Perseus molecular cloud. We aim to explore the fast rotation (in the time-scales of hours) in Very Low Mass stars (VLMs) including Brown Dwarfs (BDs). From a sample of 177 light-curves using our new I-band observations, we detect new photometric variability in 22 young M-dwarfs including 6 BDs, which are bonafide members in IC 348 and well-characterized in the spectral type of M-dwarfs. Out of 22 variables, 11 M dwarfs including one BD show hour-scale periodic variability in the period range 3.5 - 11 hours and rest are aperiodic in nature. Interestingly, an optical flare is detected in a young M2.75 dwarf in one night data on 20 December 2016. From the flare light curve, we estimate the emitted flared energy of 1.48 $\times$ 10$^{35}$ ergs. The observed flared energy with an uncertainty of tens of per cent is close to the super-flare range ($\sim$ 10$^{34}$ ergs), which is rarely observed in active M dwarfs., 12 pages, 5 figures

We present here identification and characterization of the young stellar population associated with an active star-forming site Sh2-242. We used our own new optical imaging and spectroscopic observational data, as well as several archival catalogs, e.g., Pan-STARRS 1, $Gaia$ DR2, IPHAS, WIRCam, 2MASS, and $Spitzer$. Slit spectroscopic results confirm the classification of the main ionizing source BD+26 980 as an early-type star of spectral type B0.5 V. The spectrophotometric distance of the star is estimated as 2.08 $\pm$ 0.24 kpc, which confirms the source as a member of the cluster. An extinction map covering a large area (diameter $\sim$ 50') is generated with $H$ and $K$ photometry toward the region. From the map, three distinct locations of peak extinction complexes ($A_{V}$ $\simeq$ 7$-$17 mag) are identified for the very first time. Using the infrared color excess, a total of 33 Class I and 137 Class II young objects are classified within the region. The IPHAS photometry reveals classification of 36 H$\alpha$ emitting sources, which might be class II objects. Among 36 H$\alpha$ emitting sources, 5 are already identified using infrared excess emission. In total, 201 young objects are classified toward S242 from this study. The membership status of the young sources is further windowed with the inclusion of parallax from the $Gaia$ DR2 catalog. Using the optical and infrared color-magnitude diagrams, the young stellar objects are characterized with an average age of $\sim$ 1 Myr and the masses in the range 0.1$-$3.0 $M_\odot$. The census of the stellar content within the region is discussed using combined photometric and spectroscopic data., Comment: 17 pages, 12 figures, Published in the Astronomical Journal

We present the results of flux density, spectral index, and polarization intra-night monitoring studies of a sample of eight optically bright blazars, carried out by employing several small to moderate aperture (0.4\,m to 1.5\,m diameter) telescopes fitted with CCDs and polarimeters located in Europe, India, and Japan. The duty cycle of flux variability for the targets is found to be $\sim 45$ percent, similar to that reported in earlier studies. The computed two-point spectral indices are found to be between 0.65 to 1.87 for our sample, comprised of low- and intermediate frequency peaked blazars, with one exception; they are also found to be statistically variable for about half the instances where `confirmed' variability is detected in flux density. In the analysis of the spectral evolution of the targets on hourly timescale, a counter-clockwise loop (soft-lagging) is noted in the flux-spectral index plane on two occasions, and in one case a clear spectral flattening with the decreasing flux is observed. In our data set, we also observe a variety of flux-polarization degree variability patterns, including instances with a relatively straightforward anti-correlation, correlation, or counter-clockwise looping. These changes are typically reflected in the flux-polarization angle plane: the anti-correlation between the flux and polarization degree is accompanied by an anti-correlation between the polarization angle and flux, while the counter-clockwise flux-PD looping behaviour is accompanied by a clockwise looping in the flux-polarization angle representation. We discuss our findings in the framework of the internal shock scenario for blazar sources., MNRAS accepted

Porphyrias are rare, genetically inherited group of disorders. The most common disorder among acute porphyrias are the acute intermittent porphyria, which occurs due a defect of the enzyme porphobilinogendeaminase, presenting commonly with a triad of symptoms: visceral abdominal pain, neurological dysfunction and psychiatric disturbances. Non specific myriad of symptoms causes a diagnostic confusion and delay, leading to multiple investigations, unnecessary treatment interventions, high cost of management, with frequent visits to emergency room and a prolonged ward stay. A more perplexing picture appears due to the absence of hard physical findings, and the patients get dismissed for years as “Functional”, Malingerers, Mentally ill. In underdeveloped countries, owing to limited investigative procedures, costly laboratory investigations, poor socio-economic status, much reliance on clinical judgment is required.

We report here CCD $I$-band time-series photometry of a young (2$-$5 Myr) cluster NGC 2282 to identify and understand the variability of pre-main-sequence (PMS) stars. The $I$-band photometry, down to $\sim$ 20.5 mag, enables us to probe the variability towards the lower mass end ($\sim$ 0.1 M$_\odot$) of the PMS stars. From the light curves of 1627 stars, we identified 62 new photometric variable candidates. Their association with the region was established from H$\alpha$ emission and infrared (IR) excess. Among 62 variables, 30 young variables exhibit H$\alpha$ emission, near-IR (NIR)/mid-IR (MIR) excess or both, and they are candidate members of the cluster. Out of 62 variables, 41 are periodic variables with the rotation rate ranging from 0.2 to 7 days. The period distribution exhibits a median period at $\sim$ 1-day as in many young clusters (e.g., NGC~2264, ONC, etc.), but it follows a uni-modal distribution unlike others having bimodality with the slow rotators peaking at $\sim$ 6$-$8 days. To investigate the rotation-disk and variability-disk connection, we derived NIR excess from $\Delta$(I$-$K) and MIR excess from $Spitzer$ [3.6]$-$[4.5] $\mu$m data. No conclusive evidence of slow rotation with the presence of disks around stars and fast rotation for diskless stars is obtained from our periodic variables. A clear increasing trend of the variability amplitude with the IR excess is found for all variables.

The lowland area of southern Vietnam contains a high diversity of corticolous, crustose lichens, particularly in the family Graphidaceae. Two species, Acanthothecis verrucosa S. Joshi, Upreti & Hur and Graphis exuta S. Joshi, Upreti & Hur, are described new to science. Acanthothecis verrucosa is characterized by a verrucose, olive green thallus containing irregular to shortly lirellate apothecia, hyaline to brownish proper exciple apically lined by robust periphysoids, muriform ascospores, 30–70 × 15–20 μm, and the presence of psoromic and subpsoromic acids. Graphis exuta is characterized by a smooth, greenish white thallus, simple lirellae lacking thalline margin, entire labia coarsely white pruinose towards slit, muriform ascospores, 20–35×10–13 μm, and norstictic acid in the thallus. A new name, Acanthothecis yokdonensis S. Joshi & Hur, is proposed here for the species Acanthothecis salazinica S. Joshi & Hur, a later homonym of A. salazinica van den Boom & Sipman. In addition, 34 species from Vietnam are newly reported. A world key to the group of Graphis species characterized by short, simple and sessile lirellae lacking or with basal thalline margins (nuda-morph) is presented.