Stellar Q3 Helps TCS Hit 25 Bn in Annual Revenue

Stellar Q3 Helps TCS Hit $25 Bn in Annual Revenue

Mumbai, January 12, 2022: Tata Consultancy Services (BSE: 532540, NSE: TCS) announced its consolidated financial results as per Indian Accounting Standards (Ind AS) and International Financial Reporting Standards (IFRS) for the quarter ending December 31, 2021. Quarterly Highlights for December 2021

Revenues were $6. 524 billion, up 14. 4% year-on-year, up 15. 4%CC year-on-year

Operating margin was industry-leading at 25%, down 1. 6% year-on-year
Net income was $1. 303 billion, up 10. 5% year-on-year, and net income margin was 20
Strong customer numbers: 10 new customers over $100 million (58 total), 21 new customers over $50 million (118 total).
Cash from operations was 111. 1% of net income.
Net headcount increased by 28, 238, bringing headcount to 556, 986
Diversity and inclusion: Female headcount topped 200, 000, 68% increase in female senior management from 2016-21 | Employees represent 156 nationalities
Building G& T workforce: 100, 000+ market-relevant skills acquired in Q3 | 38, 000+ contextual masters identified
LTM's IT services division attrition rate of 15. 3%, lowest in the industry
Board recommends share buyback of INR 18, 000 crore at ₹ 4, 500 per share.
Dividend per share: 7. 00 | Record date: January 20, 2022 | Payment date: February 07, 2022
Rajesh Gopinathan, Chief Executive Officer and Managing Director, said: "Our continued growth momentum is a validation of our collaborative, inside-out approach to our clients' business transformation needs. Our engagement model, end-to-end capabilities and executional approach to problem-solving are highly valued by our clients. While they chart their innovation and growth journey, we also help them execute new-age operating model transformations that support their journey."

N Ganapathy Subramaniam, Chief Operating Officer and Executive Director, said: "We remain focused on organic growth and developing the people, methodologies and toolkit that can keep up with the ever-evolving technology landscape. This, along with contextual knowledge, passion and commitment of thousands of TCS employees, enabled us to deliver cutting-edge solutions during the quarter and help clients accelerate their speed to value. We are also pleased to have crossed yet another important milestone in our journey by crossing the $25 billion revenue milestone in FY21."

According to Samir Sexia's highest finance officer (CFO): "The sustainable investment in human resources has achieved powerful growth despite the severe supply environment. Lon g-term human resources. In addition to continuing to focus on training, we are also working on tactical measures to alleviate the replacement of human resources, and to relieve costs and manage employee expenses. I exercised the means.

By industry, all industries grow from mi d-10 % to the second half. Retail / CPG (up 20. 4 %), BFSI (17. 9 % increase), and manufacturing (18. 3 % increase) have led growth. Technology and services increased by 17. 7%, life science & health care increased 16. 3%, and communication and media increased 14. 4%.

Q3 Segment Highlights**

In the major market market, North America (increased 18%) and European continents (increased 17. 5%) have led to growth, up 12. 7%in the UK. In emerging markets, Latin America (up 21. 1%) and India (up 15. 2%) have led growth, following the Middle East, Africa (up 6. 9%) and Asia Pacific (up 4. 3%).

In the third quarter of the service, it became clear that companies tend to actively invest in technology and initiatives for lon g-term growth. Cloud, cyber security, consulting & service integration, IoT & digital engineering were driven, and a wide range of growth was seen in all services.

Consulting and services integrated C & Amp; Si continues to focus on client growth and transformation initiatives with aggressive proposals that combine knowledge, skills, and domain expertise in accordance with the context of TCS. The service is integrated. Cloud strategy & transformation, customer experience, finance and shared service transformations have led the growth in the current quarter.

Cloud Platform Services: Corporate accelerating cloud introduction accelerating application transformations, modernization of IT landscape, migration to hybrid clouds, and data modernization on the cloud. TCS won AWS 2021 Rising Star Partner of the Year (GSI, USA) and AWS Application Transformation and Migration Partner of the Year (Anz).
Digital Transformation Service: The main theme of G & Amp; T in the third quarter was connected enterprise, product innovation, customer experience transformation, and security services. With engineering and IoT services, customers can acquire ful l-time traceability of products throughout the value chain, manage assets, innovate products, redesign factories, and improve prediction and business efficiency. This led the growth of intelligent devices, GIS, plant solutions and services. IoT, engineering, and analytics services also support customers on sustainability travel, which is an important business priority. Digital ERP journey using TCS Crystallus ™ supports digital transformation and business value for companies. The change in Oracle Cloud and Niche SaaS has led the quarterly growth. TCS's Cyber Defense Suite and Global Thread Management Centers provides security services that are agile and localized, such as ransomware measures, cloud security, and managed security services. I led 。
Demands have been promoted by customers seeking outsourcing IT and business operations to increase the agility of the Cognitive Business Operation Business, the recovery of operations, and cost efficiency. The growth in the third quarter was led by Enterprise BPS, infrastructure transformation and automation services. MFDM ™ and Cognix ™ continue to provide strong relevance to the market and provide joy to customers.
** Growing on a constant currency basis compared to the same period of the previous year

As of December 31, 2021, TCS applied for 6, 396 patents, including 227 applications filed during the quarter, and obtained 2, 201 patents.

Research and Innovation

In the third quarter, TCS achieved a new diversity milestone, with more than 200, 000 female employees. The number of employees increased by 28, 238 on a net increase, and the total number of employees as of December 31, 2021 was 556, 986. Global employees with 156 countries are working due to the policy of hiring local human resources around the world.

Human Resources

The company continued to invest in organic human resource development. In the third quarter, TCS employees learned more than 100, 000 marke t-related skills. 32. 3%of the recruitment position was fulfilled by skill improvement / cros s-skilled up. Overall 38, 000 contextual masters have been identified throughout the organization, which is a larg e-scale specialist group that has been developed within the company, and has supported the advancement of TCS for growth and transformation opportunities.

Sustainable investment in organic human resources, advanced workplace policies, and lively corporate culture that foster creativity and fostering creativity, have recorded the highest human resource retention rate in the class for a long time. The third quarter of the IT service division (LTM) was 15. 3%.

"The ability to attract and maintain excellent human resources around the world is the center of the success of the TCS business and the source of competitive differentiation. We continue to set a new record in acquiring human resources. In the first half, in the third quarter, we will continue to be a benchmark of the industry. Continue investing in, the most exciting position is the company's i n-house candidates, providing global development opportunities, providing a quick career path linked to learning, and more than 110, 000 employees. By providing the opportunity to promote, we have been able to maintain the best human resources and overcome the issues on the supplier, "said Mirind Rackad, HRO.

Business leadership

Awards and Recognition

The outstanding business growth of TCS, the position of the No. 1 sales in the UK, the No. 1 customer satisfaction, the number of customer satisfaction, and the community initiatives have been evaluated, and has been elected to the UK Super Brand for the seventh consecutive year.

The market is highly evaluated, digital, and business growth is evaluated, and is certified as a Singapore super brand.
In 2021, at the ITSMA Marketing Excellence Awards, he won the Diamond Award in two categories in the "ABM Program Fixation" and "Establishing Executive Engagement".
In 2021, three awards in Linkedin Best Employer Brand, Best Culture of Learning, and Diversity Champion.
Economic Times Human Capital Awards 5 Awards: Communication Strategic Division Award, Cultural Creation Division Award for Continuing Learning and Skills, Innovation and Design Thinking Division Excellence Award, Personnel Digital Transformation Division Exposition Award , Professional Recruitment Division Excellence Award.
Won the World Leadership Congress Award for all women's business process services and IT center worl d-class operations in the Riyado of Saudi Arabia.
The brand's reputation in the Middle East was evaluated and won the 2021 Economic Times Best Brand of the UAE Award.
Innovation and intellectual property:

In 2021, he won the Best Patent Portfolio Award in the large corporate division of the Indian Industrial Federation Industrial Intelligence Award.

Received the pioneer in promoting innovation and healthy intellectual property (IP) ecosystem (IP) Ecosystem, won the 2021 ASSOCHAM IP Excellence Award.
Awarded Enterprise Blockchain Awards 2021 from the Blockchain Research Institute.
In the IoT Global AWARDS 2021, TCS Digiflex won two awards in the car, transportation, and travel department, and TCS SMART STORE won two in the retail, marketing hospitality division.
The TCS ADD REGULATORY platform has won the Excellence Award in the Ancillary Pharma Services category of India Pharma Awards 2021.
TCS's Digital Twin Platform for Shaipem has won the Excellence Award in the Energy and Public Interest Business Division, and has also won the Excellence Award in the South European region.
In 2021, in the 2021, the Best Prize in Crisis Management Division (TCS Vaccination Solution) and the Best Awards (TCS Time Seat App) in the Brandon Hall Group Excellence in Technology Awards Award.
partner

TCS won the following awards from the Technology Alliance Partner:

In Australia and New Zealand's AWS Partner Awards, we won the Application Transformation and Migration Partner of the Year.

In 2021, he won the IFS Solutions Partner of the Year and IFS Service Partner of the Year (Enterprise Category) at the IFS Partner of the Year Awards.
BMC Partner of The Year Awar d-Cognitive Automation was awarded in BMC Service Provider Exchange (SPEX).
2021 Partner of the Year Award by Smart Message
Powerful growt h-ID and access management partner of the year 2021 by Cyberres, a business line of microfocus.
A solution introduced by TCS to Sail and Trent has been awarded in the Manufacturing Transformation section and Game Changer category of SAP ACE AWARDS 2021.
In the Red Hat Partner Awards, he won the highest award in the GAME CHANGE R-Game Change r-Enterprise business category in India and South Asian.
Tata Consultant Services, which provides IT services, consulting, and business solutions, has been cooperating with the world's largest company for over 50 years. TCS provides consulting led, cognitive power, business, technology, engineering services and solution integrated portfolios. This is provided through its own Location Independent Agile ™ Delivery model, which is recognized as an outstanding benchmark in software development.

About Tata Consultancy Services

The formation of stars and planets includes not only accumulation of substances called adhesions, but also exhausted by ultrasonic jet that can be several percent. The most powerful jet is related to the youngest star because it has a correlation between adhesion and jet activity, and young stars are rapidly acquired at most of their masses in early stages. However, this period overlaps when the primitive stars and their surroundings are hidden behind any grade decline. Mill i-wave negotiatives can be searched for this stage, which is only for the most lo w-temperature components. There is no information about the highest temperature (1, 000 k k or more) components of the jet, that is, the atomic gas, ionized gas, and high temperature molecular gas that is considered to make the jet spine. To detect such thorns, it is necessary to observe infrared rays that can transmit dust coverage. Here, we will report the nea r-infrared observation of Helvich Halo 211 by James Webb Space Telescope. These observations revealed a large amount of release from high temperature molecules, explaining the origin of the "Green Father" 4, 5, 6, 7 discovered by Spitzer Space Telescope 8 about 20 years ago. It turns out that this outflow flow is transmitted slowly compared to the evolved outflow current, and surprisingly, there are few traces of atoms or ionized light, and the spine of this outflow is almost pure. It suggests that it is a molecule.

Outflows from the youngest stars are mostly molecular

July 21, 2022

Insights into the collapse and expansion of molecular clouds in outflows from observable pressure gradients

October 16, 2019 Article

Meridional flows in the disk around a young star

August 19, 2020

Cold gas in the Milky Way’s nuclear wind

Helbig Halo 211 (hereafter, HH211) is a distance of 321 ± 10 PCs (Ref. HH211 is the youngest, the youngest, closest primitive star style, which is the youngest, the youngest, closest to the Perseus seat. , 11, the ideal target of the terrestrial telescope (northwest) is the ideal target of the terrestrial infrared observation with hig h-resolution of James Webb Space Telescope (JWST). A huge shock wave with a transition (southeast) and a shock wave

Main

(Literature 10, 12) and CO millimeter wave line 13, each of the huge red transitions (northwest) and blu e-sided shock (southeast), and a hollow structure, and in SIO 14. A kno t-shaped bipola jet was found. At the center is a primitive star in class 0 called HH 211-mm.₂There is only mass, but 0. 2 m_⊙It is in the middle of being settled from the gas and dust torus 13._⊙The 1st cycle warranty time observation program by the US Aeronautics and Space Agency (NASA) / European Space Organization (ESA) / Canada Space Organization (CSA) JWST (PID) 1257, chief researcher (Pi) T. P. Ray) It was composed of an image by the entire HH 211 nea r-infrared camera (NIRCAM) 16, and an observation by nea r-infrared floodle device (NIRSPEC) 17 and a medium infrared spectroscope (NIRSPEC) 17. P. Ray) was imaged throughout HH 211 by nea r-infrared camera (NIRCAM) 16, and the integrated field of sight of the south east leaf by nea r-infrared spectroscopy (NIRSPEC 17) and medium infrared dimeromes (MIRI 18). Here are the preliminary results obtained from the first NIRCAM and NIRSPEC observations.

The three-color image (Fig. 1) of NIRCAM (Fig. 1) is a series of spatial resolution capacity, about 5-10 times higher than any of the previous images, with a series of bausing shocks between southeast and northwest (lower left) and northwest (upper right). So, it has been shown in more detail. Overall, the light emitting is red, from the color synthesis F470N filter, 4. 69 μm H

It is dominated by the 0-0 S (9) line. Other H₂O (5) transitions, etc.), and other molecules, such as basic rotation vibration radiation from C (see below and method).₂Figure 1: JWST image of HH 211.

NIRCAM synthesis images of F335m (blue), F460m (green), and F470N (red). In order to compress the dynamic range, the strength of each image was contraryated before being synthesized. The northwest of the outflow is known for the red transition, and the southeastern part is a blue shift. Some H for the middle band F335M filter

In particular, the 3. 23 μm v = 1-0 O(5) line and the continuum nebula. The mid-band F460M filter contains the 0-0 S(9) line at 4. 69 μm, many lines of CO rovibrational band head emission, and the continuum nebula. The narrow-band F470N filter is dominated by the H₂line at 4. 69 μm. Note the shift in scattered light to longer wavelengths as we approach the protostar in the center of the dark lane. The lack of red light toward the protostar is due to the narrowness of the F470N filter. The azimuth and the scale of the projection in astronomical units (AU) (assuming a distance of 321 pc) are shown at the bottom right.₂The inner jet is seen to wriggle mirror-symmetrically on either side of the central protostar. This is consistent with smaller-scale observations in SiO (ref. 14), suggesting that the protostar may be an unresolved binary 19 . The protostar itself is still too buried to be detected at these wavelengths, but it is likely illuminating the conical rim of the outflow cavity through a reflection nebula. Most of this blue emission fades to green as it approaches the protostar.

The rich NIRSpec (1. 7-5. 1 μm) spectrum of the apex of the southeast bow shock (Figure 2) shows a number of bright transitions from H

This spectrum contains pure rotational transitions (labeled in blue), as well as rotational-vibrational lines from v = 1 (black), v = 2 (red), and higher vibrational levels (not labeled). A notable feature of the spectrum is the large number of bright transitions in the fundamental R and P branches of CO(1-0) between 4. 3-5. 1 μm, interspersed with lines from the corresponding isotope 13CO (Figure 2, inset). Faint CO lines between 2. 29 and 2. 4 μm (due to CO overtones v=2-0, 3-1, 4-2) were also detected along with some weak [FeII] emissions (not labeled). Of note is the near absence of ionization or atomic transitions.₂Figure 2: NIRSpec spectrum of the apex of the HH211 SE bow shock.

Figure 2: NIRSpec spectrum of the apex of the HH211 SE bow shock. The most prominent H

0-0, 1-0, and 2-1 transitions are shown in blue, black, and red, respectively, and CO transitions in green. Note the presence of a secondary peak associated with the 12CO fundamental series (inset) due to the 13CO isotope. For reference, the spectral coverage of the NIRCam imaging filter is shown above the wavelength axis.₂Many years ago, it was noted that the embedded outflows imaged with the Infrared Array Camera (IRAC) on the Spitzer Space Telescope 8 showed large intensity variations across a wide range of IRAC bands. In particular, three-color images using IRAC band 1 (blue, central wavelength 3. 6 μm), IRAC band 2 (green, central wavelength 4. 5 μm), and IRAC band 4 (red, central wavelength 8. 0 μm) showed that the outflows were predominantly "green". The origin of this "faint green" emission was thought to be the H 0-0 S(9) line (ref. 20) or the CO (1-0) rovibrational line (refs. 4, 5, 6). An alternative explanation for the excess "green" emission is a mixture of H emission and scattered continuum light from the embedded young star 7. But regardless of its origin, the detection of such "green" emission21 was considered a very effective way to track outflows from low-mass and even more massive buried young stars22, not only by Spitzer but also by the subsequent Wide-field Infrared Survey Explorer (WISE) mission23.

A combined analysis of NIRCam and NIRSpec observations of HH211 revealed that the pronounced excess seen in Spitzer IRAC band 2 (4. 5 μm) is mainly due to the fundamental roto-vibrational emission of CO.₂Figure 3 shows a three-color composite image of HH 211. On the far right is a composite image of Spitzer IRAC bands 1, 2, and 4, with the jet clearly in green. On the far left, the JWST F335M image is replaced with Spitzer band 1 blue, i. e. 3. 35 μm to 3. 6 μm, and the JWST F460M image is replaced with Spitzer band 2 green, i. e. 4. 6 μm to 4. 5 μm, with IRAC band 4 again in red. The resulting colors (derived using the same intensity scale settings) are the same, despite the wider bandwidth of the IRAC filters and dramatically different spatial resolutions of the telescopes.

Figure 3: Color match of the "green haze" of HH 211.₂a, JWST NIRCam F335M (blue), F460M (green) and Spitzer IRAC band 4 (red) images combined. The colors match very well, despite the different filter set bandwidths and telescope spatial resolutions.

To examine the location of the CO (1-0) emission along the flow and the intensity of the CO (1-0) emission line relative to the brightest H line (the 0-0 S(9) line at 4. 69 μm) in the F460M filter, we used the 'CO-H

The color image (Fig. 4 and the method) shows a place where Co flux is dominant (positive; bright yellow white), and con.

It shows a place where light emitting is dominant (negative; dark orange-red). The shine of the CO is the brightest in several places near the top of the bo w-shaped impact wave and the northwest bo w-shaped shock wave, and the light line of H is clearly bright along the southeast bo w-shaped shock wave.

The release of the jet is obviously the brightest in most of the bausock. The positive luminous bundle toward the hollow wall faithfully traces the light emission of F335M (blue) found in the same place in Fig. Note that there is. The existence of strong hig h-temperature CO release (temperature T or more T 1, 000 k or more) in the boat shock wave has been predicted for many years. However, in this figure, the hig h-temperature CO is only seen in the shock wave of the bow and is not seen in the jet inside, so it may be that the surrounding molecular cloud gases received from the shock wave.

Figure 4: Co-H₂Image of.₂As the negative flux grows, h₂Exhaust and positive flux have increased more pure CO emissions. See Methods for how it was made. The color bar is displayed with ERG S-1 c m-2 ARCSSe c-2. The positive flux along the hollow wall is thought to be due to continuous radiation from the primitive star.₂It is known that the outflow speed from young stars changes considerably as a function of the depth of the gravity well of the primitive star. In particular, only a small part of the mass, young, embedded astronomical objects, have a shallow gravity well for extracting energy, and may have much lower leakage than the evolved celestial bodies. 26.

HH211's driving source is considered very young, so it may be useful to check the spill speed. The image of Nircam's F212N is a 2. 12 μm V = 1-0 S (1) H color image (Fig. 4 and method) is a place where Co flux is dominant (right; bright yellow white). H₂It shows a place where light emitting is dominant (negative; dark orange-red). The shine of the CO is the brightest in several places near the top of the bo w-shaped impact wave and the northwest bo w-shaped shock wave, and the light line of H is clearly bright along the southeast bo w-shaped shock wave.

Image of.

As the negative flux grows, h₂Exhaust and positive flux have increased more pure CO emissions. See Methods for how it was made. The color bar is displayed with ERG S-1 c m-2 ARCSSe c-2. The positive flux along the hollow wall is thought to be due to continuous radiation from the primitive star.

It is known that the outflow speed from young stars changes considerably as a function of the depth of the gravity well of the primitive star. In particular, only a small part of the mass, young, embedded astronomical objects, have a shallow gravity well for extracting energy, and may have much lower leakage than the evolved celestial bodies. 26.

HH211's driving source is considered very young, so it may be useful to check the spill speed. The image of Nircam's F212N is a 2. 12μm V = 1-0 S (1) H color image (Fig. 4 and 4), where the Co flux is dominant (positive; bright yellow white).₂It shows a place where light emitting is dominant (negative; dark orange-red). The shine of the CO is the brightest in several places near the top of the bo w-shaped impact wave and the northwest bo w-shaped shock wave, and the light line of H is clearly bright along the southeast bo w-shaped shock wave.

Figure 4: Co-H

Image of.

As the negative flux grows, h

Methods

Observations and data reduction

Exhaust and positive flux have increased more pure CO emissions. See Methods for how it was made. The color bar is displayed with ERG S-1 c m-2 ARCSSe c-2. The positive flux along the hollow wall is thought to be due to continuous radiation from the primitive star.

HH211's driving source is considered very young, so it may be useful to check the spill speed. The image of Nircam's F212N is 2. 12μm V = 1-0 s (1) line H.

This image is a lower spatial resolution image taken through a 2. 12 μm filter in 2002 at an infrared meter (ISAAC) of a supe r-large telescope (VLT) of the European South Changen Written Research Organization (ESO). There are 12. Despite the difference in spatial resolution, the 2 0-year bass line guarantees a good order movement and the estimation of the tangent speed. Since the inclination angle of the outflow is close to the celestial sphere, the tangential speed is almost the same as the thre e-dimensional speed 14.

FIG. 5 is a tangent speed vector derived from the distance to the interconnection method (Methods) and the HH211. The measured speed is generally about 80-100 km S-1 in the inside (20 "or less from the primitive star), but the speed is remarkable in the northwest side, that is, in the reddish shock wave. Supplementary video 1 indicates the observed movement of HH 211.₂Figure 5: 2. 12 μm h of HH 211₂Lighting speed of light emission.₂This is a combination of 2002 ESO VLT images with our Nircam F212N images. Note that the speed of the northwest is that the speed is systematic as the distance from the primitive stars. The plotted point is in the center of the area where the unique movement is determined using a mutual associative method (Methods). If the average speed is 100km s-1, the position angle error is about ± 6 °. The faster the knot moves, the smaller the position angle error, and the larger the slower, the larger. The center is HH211-mm (right red sutra α = 03:43:03:43 56. 8054 seconds; Dediatric δ = 32 ° 00 '50. 189 ″, (J2000. 0)).

The speed of the jet knot inside is about 100km S-1, consistent with the speed observed in the inner knots of the SIO style 14. Since the northwest jet seems to be propagating faster than the associated lock shock waves, the spilled outflow that has been in red may decelerate when rushing into the parent cloud. In contrast to this, the southeast blu e-colored ghetto may have been propagated almost in a trajectory without much disturbing. The fact that the environment has asymmetry of eas t-west density is backed by observations. This image shows a lower spatial resolution capable of filtering a 2. 12 μm filter in 2002 at an infrared meter (ISAAC) of the Ultr a-Large Telescope (VLT) of the European South Changian Written Research Organization (ESO). The image of 12. Despite the difference in spatial resolution, the 2 0-year bass line guarantees a good order movement and the estimation of the tangent speed. Since the inclination angle of the outflow is close to the celestial sphere, the tangential speed is almost the same as the thre e-dimensional speed 14.

Figure 5: 2. 12 μm h of HH 211₂Lighting speed of light emission.₂This is a combination of 2002 ESO VLT images with our Nircam F212N images. Note that the speed of the northwest is that the speed is systematic as the distance from the primitive stars. The plotted point is in the center of the area where the unique movement is determined using a mutual associative method (Methods). If the average speed is 100km s-1, the position angle error is about ± 6 °. The faster the knot moves, the smaller the position angle error, and the larger the slower, the larger. The center is HH211-mm (right red sutra α = 03:43:03:43 56. 8054 seconds; Dediatric δ = 32 ° 00 '50. 189 ″, (J2000. 0)).₂The speed of the jet knot inside is about 100km S-1, consistent with the speed observed in the inner knots of the SIO style 14. Since the northwest jet seems to be propagating faster than the associated lock shock waves, the spilled outflow that has been in red may decelerate when rushing into the parent cloud. In contrast to this, the southeast blu e-colored ghetto may have been propagated almost in a trajectory without much disturbing. The fact that the environment has asymmetry of eas t-west density is backed by observations. This image is a lower spatial resolution image taken through a 2. 12 μm filter in 2002 at an infrared meter (ISAAC) of a supe r-large telescope (VLT) of the European South Changen Written Research Organization (ESO). There are 12. Despite the difference in spatial resolution, the 2 0-year bass line guarantees a good order movement and the estimation of the tangent speed. Since the inclination angle of the outflow is close to the celestial sphere, the tangential speed is almost the same as the thre e-dimensional speed 14.₂FIG. 5 is a tangent speed vector derived from the distance to the interconnection method (Methods) and the HH211. The measured speed is generally about 80-100 km S-1 in the inside (20 "or less from the primitive star), but the speed is remarkable in the northwest side, that is, in the reddish shock wave. Supplementary video 1 indicates the observed movement of HH 211.₂Figure 5: 2. 12 μm h of HH 211

Proper motion and tangential velocity measurements

Lighting speed of light emission.₃This is a combination of 2002 ESO VLT images with our Nircam F212N images. Note that the speed of the northwest is that the speed is systematic as the distance from the primitive stars. The plotted point is in the center of the area where the unique movement is determined using a mutual associative method (Methods). Assuming the average speed is 100km s-1, the position angle error is about ± 6 °. The faster the knot moves, the smaller the position angle error, and the larger the slower, the larger. The center is HH211-mm (right red sutra α = 03:43:03:43 56. 8054 seconds; Dediatric δ = 32 ° 00 '50. 189 ″, (J2000. 0)).₃The speed of the jet knot inside is about 100km S-1, consistent with the speed observed in the inner knots of the SIO style 14. Since the northwest jet seems to be propagating faster than the associated lock shock waves, the spilled outflow that has been in red may decelerate when rushing into the parent cloud. In contrast to this, the southeast blu e-colored ghetto may have been propagated almost in a trajectory without much disturbing. The fact that the environment has asymmetry of eas t-west density is backed by observations.

The characteristics of the light emission seen in the jet are thought to be due to the "internal work", that is, the impact of hig h-speed jet substances colliding with the lo w-speed substance in front. Therefore, it is not an absolute speed to determine the shock speed 27, but the speed difference between these components, probably several tens of km s-1. Therefore, the jet speed of the observed 100km S-1 jet may not be the actual impact speed. In addition, such a hig h-speed impact will quickly dissolve the molecular 28 we are observing, creating abundant ionization and atomic species that we have not observed. Therefore, the shock wave that exists in the outflow flow of HH 211 is likely to be at low speed. An interesting feature of such a shock is that it has a low ability to destroy dust grains. This guarantees that the outflow from a very young primitive star, such as HH 211-mm, not only return gas to interconnated substances, but also includes dust treated with the primitive stars. Dust is at least partially destroyed in an evolved outflow.

Data availability

Finally, the important conclusion of this study is that, mainly obtained from our NIRSPEC data, the jet from the early primitive stars is a molecular beam that moves slowly. The characteristics of the light emission seen in the jet are thought to be due to the "internal work", that is, the impact of hig h-speed jet substances colliding with lo w-speed substances in front. Therefore, it is not an absolute speed to determine the shock speed 27, but the speed difference between these components, probably several tens of km s-1. Therefore, the jet speed of the observed 100km S-1 jet may not be the actual impact speed. In addition, such a hig h-speed impact will quickly dissolve the molecular 28 we are observing, creating abundant ionization and atomic species that we have not observed. Therefore, the shock wave that exists in the outflow flow of HH 211 is likely to be at low speed. An interesting feature of such a shock is that it has a low ability to destroy dust grains. This guarantees that the outflow from a very young primitive star, such as HH 211-mm, not only return gas to interconnated substances, but also includes dust treated with the primitive stars. Dust is at least partially destroyed in an evolved outflow.

Code availability

Finally, the important conclusion of this study is that, mainly obtained from our NIRSPEC data, the jet from the early primitive stars is a molecular beam that moves slowly. The characteristics of the light emission seen in the jet are thought to be due to the "internal work", that is, the impact of hig h-speed jet substances colliding with the lo w-speed substance in front. Therefore, it is not an absolute speed to determine the shock speed 27, but the speed difference between these components, probably several tens of km s-1. Therefore, the jet speed of the observed 100km S-1 jet may not be the actual impact speed. In addition, such a hig h-speed impact will quickly dissolve the molecular 28 we are observing, creating abundant ionization and atomic species that we have not observed. Therefore, the shock wave that exists in the outflow flow of HH 211 is likely to be at low speed. An interesting feature of such a shock is that it has a low ability to destroy dust grains. This guarantees that the outflow from a very young primitive star, such as HH 211-mm, not only return gas to interconnated substances, but also includes dust treated with the primitive stars. Dust is at least partially destroyed in an evolved outflow.

Change history

References

Finally, the important conclusion of this study is that, mainly obtained from our NIRSPEC data, the jet from the early primitive stars is a molecular beam that moves slowly.
On August 28, 2022, JWST's NIRCAM was the entire HH211 field, a part of HH211's southeast bo w-shaped shock wave (line in Fig. 2) at NIRSPEC, and HH211 warranty time observation program (PI: Ray, ID 1257). It was observed as part. Nircam16 observes the red light and near-infrared wavelength range of 0. 6-5. 0 μm at the same time on two channels, a short wavelength (SW) channel (0. 6-2. 3 μm) and a long wavelength (LW) channel (2. 4-5. 0 μm). Masu. Each two modules (a and b) operate in parallel. The field of view of each module is 2. 2 '× 2. 2' (area of 4. 84 square arcs), and these are separated by the gap of about 44 ″. The entire field of each channel is about 9. 7 square areas. In the SW channel. , Approximately 5 "gaps separate the four detectors that make up each module. Both modules on each channel operate with the same narrow band, middle band, and wide bandwidth filter. The image resolution of the SW channel is about 31 mids per pixel, and the LW channel is about 63 mm seconds per pixel. In the HH211 field observation by Nircam, the narrow and middle band filters described in the expansion data Table 1 were used. This table includes the basic characteristics of the filter, the bright line to cover, and the related spatial resolution. In some cases, it was also considered to be used for continuous light subtraction purposes. Except for F210m/F460M and F162M + F150W2/F335M, all shorts and long filters were combined, using a bright1 reading pattern with one integral of eight groups, using one integral of 4 groups. For the combination of the Intramodulex pattern length/ short filter, we performed the Diza exposure four times with the Standard subpixel diza type.
All Nircam data uses the JWST Pipeline V. 1. 7. 2 (Ref. 31), each of the V. 11. 16. 10, Calibration Reference Data System (CRDS) and CRDS context. Using it It has been reduced. First, using Detector1pipeline and Image2pipeline, processing unable to calibration, then using ImagePipeline to synthesize the mosaic related to specific filters.
However, there were two problems in the created mosaic. As expected, the pipelin e-processed images were suffering from 1/F banding noise 32, for any difference. This impact is more prominent in the narrow band image than the medium band image. In particular, the nircam reading system mainly causes a noise space correlation along a hig h-speed reading direction, that is, a detector column, and creates a banding. In order to reduce the 1/f noise component, an additional correction was performed based on the ROEBA tools implemented each row, and the Detector1Pipeline was r e-executed. However, in consideration of the angle scale of HH211, a very careful attention was paid to the pixels covered in the extended emissions when determining the median 1/f noise used in the correction was determined. This could prevent excessive extraction of the actual extend light emission. In some cases, the extend light emission covered one or one row of the amplifier, so it was impossible to correct each and every amplifier. In such a case, we only returned to the correction for each line. Using Image2pipeline and Image3pipeline, these newly modified slope files have been reprinted and the mosaic is reproduced. After removing the band noise to the final image using the GIMP G'mic-QT, the image was synthesized to synthesize the image.
The second problem was a slight su b-pixel shift in relative astrometry between filter mosaics. To take these into account, the fitting function of stars with a medium brightness in the field was fitted with a tw o-dimensional Gaussian to determine the sky coordinates. Using the center point, offset correction was performed for the F460M filter.
The images used as blue, green, and red in Fig. 1 are F335m (medium band filter centered on 3. 365 μm, several H.
Line (including 3. 323 μm 1-0 O (5) transition), F460m (middle band filter centered on 4. 624 μm, CO basic wave radiation and H₂0-0 S (9) Transition), F470N (H , but there were two problems in the created mosaic. As expected, the image of the pipeline-processed image is a degree of difference. The effect of the 1/F banding noise 32 is more prominent in the nircam reading system than the medium band image. In order to reduce the space correlation of the noise and reduce the banding, the ROEBA tools are implemented for each row, and the Deter1Pipeline is r e-executed. However, in consideration of the angle scale of HH211, the pixels covered in the extended emission are paid for the time being determined. However, in some cases, the excessive extension of the extension was covered by the extension, so it is impossible to correct each row of the amplifier. In such a case, we used these new slope files to recreate the modified slope files only to the correction. After removing the band noise to the final image usin g-Qt, the image was synthesized and colored.
The second problem was a slight su b-pixel shift in relative astrometry between filter mosaics. To take these into account, the fitting function of stars with a medium brightness in the field was fitted with a tw o-dimensional Gaussian to determine the sky coordinates. Using the center point, offset correction was performed for the F460M filter.
The images used as blue, green, and red in Fig. 1 are F335m (medium band filter centered on 3. 365 μm, several H.
Line (including 3. 323 μm 1-0 O (5) transition), F460m (middle band filter centered on 4. 624 μm, CO basic wave radiation and H
0-0 S (9) Transition), F470N (H, but the created mosaic had two problems. As expected, the pipeline-processed images are 1, 1. The impact of the Banding noise 32 is more prominent in the nircam reading system than the medium band image. In order to reduce the space correlation and reduce this 1/f noise, an additional compensation is performed based on the amplifier tool 32. Considering the angle scale of HH211, the pixels covered in the extended emission were paid to the pixels that are used in the correction. In some cases, the extend light was covered by one or one row of amplifier in some cases. In such a case, the gimp of the gimp was reproduced by using the newly corrected slope file using only the correction. After removing the band noise to the final image, the image was synthesized to synthesize the image.
The second problem was a slight su b-pixel shift in relative astrometry between filter mosaics. To take these into account, the fitting function of stars with a medium brightness in the field was fitted with a tw o-dimensional Gaussian to determine the sky coordinates. Using the center point, offset correction was performed for the F460M filter.
The images used as blue, green, and red in Fig. 1 are F335m (medium band filter centered on 3. 365 μm, several H.
Line (including 3. 323 μm 1-0 O (5) transition), F460m (middle band filter centered on 4. 624 μm, CO basic wave radiation and H
0-0 S (9) Including transition), F470N (H)
0-0 S (9) Transition at 4. 695 μm). Only a small part of the nircam module A and B fields is displayed here, and the rest is mainly the two almost parallel flows from IC348 mms and the bo w-shaped shock wave of HH211. You can see that the outflow flow from other nearby stars in the nearby noodles, such as the outflow of the north and south, is intersecting. The latter may be related to the specific exercise research below.
According to NIRSPEC observations, G235H /F170LP (1. 66-3. 05 μm; λ /δ λ = 2, 700) and G295H /F290LP (2. 87-5. 14 μm; Approximately 8 "x 11" areas contained were mapped in total exposure time 6, 336 seconds (insertion in Fig. 2). Similar to the 'Leakcal' observation for the leak correction of microsutter assembly, tw o-point noding was applied. The data was reduced and calibrated using JWST Pipeline V. 1. 8. 2, and was acquired from Mikulski Archive for Space Telescopes. The spectrum extraction and analysis were used using Common Astronomy Software Applications 33 and Image Redaction and Analysis Facility 34.
The flux comparative spectrum shown in FIG. 2 is the area of 1 "x 1" centered on the outermost southeast bo w-shaped shock wave (α = 3 h 43 min 59. 9 s; δ = 32 ° 00 '34. 29 ". It is based on the area of 1 "x 1" centered on, (J2000. 0)).
CO vs. H
Was subtracted twice.
) I pulled it twice from the image.
) H by drawing twice from the image of)
The light emitting has a negative flux. It is common for CO to use the F466N filter image (Extended Data Table 1), but the F466N filter image contains only a few low J rotation R branches of CO, so all flux of CO. Note that the estimation is very limited. For checking, F4. 1 co/h
The line flux ratio was derived from NIRSPEC data, and the ratio was compared with the same position obtained from the nircam image, that is, at the peak of Bow Shock. The obtained values were 4. 33 ± 0. 09 and 4. 5 ± 0. 3, matching within the uncertainty.
To measure the appropriate exercise of the structure during the outflow of HH211, a mutual correlation of the leaked section is required. It turned out that this was much more effective than simply tracking bright pixel movements over time. Furthermore, since the spatial resolution of 2. 12μm images of ESO VLT and JWST has a large difference from 0. 6 "vs 0. 08" (Supplementary Video 1 and Extended Data Fig. 1), the hig h-resolution images are converted to the other resolution. Then, applying mutual correlation technology is better than pixel tracking. The selection of areas used for mutual correlation is ultimately restricted by (relatively) resolution of the ESO VLT image: to trace all small structures found in Jwst images. You have to wait for the second epoch for JWST observation. FIG. 2 is a plot of the measured contact speed and the distance from the astronomical object to compare with FIG. 5. Note that the movement to the northwest is clearly slow. The density asymmetry in the east and west, and the darker gas in the west was backed by the mill i-band observation. In particular, a high-density filament is seen on the west side, that is, on the reddish transition side of HH 211-mm, NH in H 13 Co +.
(See 13). In addition, recent NH
The observation shows a clear increase in the turbulent movement along the direction of the HH 211 northwest jet, that is, a large line width, which is deposited from the outflow 35 due to deceleration. It suggests a possibility. Another number obtained from the one in which the projection distance is divided by the tangent speed is the mechanical time scale of the system. This is within 10-4 years, the theoretical age of HH211-mm. HH211 Measure the appropriate movement of the structure during the outflow requires the intercon correction of the leaked section. It turned out that this was much more effective than simply tracking bright pixel movements over time. Furthermore, since the spatial resolution of 2. 12μm images of ESO VLT and JWST has a large difference from 0. 6 "vs 0. 08" (Supplementary Video 1 and Extended Data Fig. 1), the hig h-resolution images are converted to the other resolution. Then, applying mutual correlation technology is better than pixel tracking. The selection of areas used for mutual correlation is ultimately restricted by (relatively) resolution of the ESO VLT image: to trace all small structures found in Jwst images. You have to wait for the second epoch for JWST observation. FIG. 2 is a plot of the measured contact speed and the distance from the astronomical object to compare with FIG. 5. Note that the movement to the northwest is clearly slow. The density asymmetry in the east and west, and the darker gas in the west was backed by the mill i-band observation. In particular, a high-density filament is seen on the west side, that is, on the reddish transition side of HH 211-mm, NH in H 13 Co +.
(See 13). In addition, recent NH
The observation shows a clear increase in the turbulent movement along the direction of the HH 211 northwest jet, that is, a large line width, which is deposited from the outflow 35 due to deceleration. It suggests a possibility. Another number obtained from the one in which the projection distance is divided by the tangent speed is the mechanical time scale of the system. This is within 10-4 years, the theoretical age of HH211-mm. To measure the appropriate exercise of the structure during the outflow of HH211, a mutual correlation of the leaked section is required. It turned out that this was much more effective than simply tracking bright pixel movements over time. Furthermore, since the spatial resolution of 2. 12μm images of ESO VLT and JWST has a large difference from 0. 6 "vs 0. 08" (Supplementary Video 1 and Extended Data Fig. 1), the hig h-resolution images are converted to the other resolution. Then, applying mutual correlation technology is better than pixel tracking. The selection of areas used for mutual correlation is ultimately restricted by (relatively) resolution of the ESO VLT image: to trace all small structures found in Jwst images. You have to wait for the second epoch for JWST observation. FIG. 2 is a plot of the measured contact speed and the distance from the astronomical object to compare with FIG. 5. Note that the movement to the northwest is clearly slow. The density asymmetry in the east and west, and the darker gas in the west was backed by the mill i-band observation. In particular, a high-density filament is seen on the west side, that is, on the reddish transition side of HH 211-mm, NH in H 13 Co +.
(See 13). In addition, recent NH
The observation shows a clear increase in the turbulent movement along the direction of the HH 211 northwest jet, that is, a large line width, which is deposited from the outflow 35 due to deceleration. It suggests a possibility. Another number obtained from the one in which the projection distance is divided by the tangent speed is the mechanical time scale of the system. This is within 10-4 years, the theoretical age of HH211-mm.
There are two main causes of the errors in the unique movement. The first is the accuracy of the registered image between ESO VLT and JWST images, and is converted from the error of the arc second to the equivalent speed of the KM S-1. The same value is used for all unique movements. Other errors are determined by the mutual association by changing the input parameters such as the size of the box and seeing how much the measured exercise changes. In some knots, the error is small because the knots are beautiful and symmetrical, but in other knots, the error increases due to the confusion with other structures that enter and exit the interconnection opening. Not all knots, but most knots have dominant registry errors. It should be noted that although the errors are accumulated, as shown in the expansion data FIG. Finally, there is a system error due to the uncertainty of the distance to HH211, but it can be ignored compared to other errors.
The reduction data of Nircam and NIRSPEC is available if there is a request from the corresponding author. The reduction data of the standard pipeline will be published in the Mast portal (https://mast. stsci. edu/portal/mashup/clients/mast/portal. html) one year after the observation date. There are two main causes of errors in the unique movement. The first is the accuracy of the registered image between ESO VLT and JWST images, and is converted from the error of the arc second to the equivalent speed of the KM S-1. The same value is used for all unique movements. Other errors are determined by the mutual association by changing the input parameters such as the size of the box and seeing how much the measured exercise changes. In some knots, the error is small because the knots are beautiful and symmetrical, but in other knots, the error increases due to the confusion with other structures that enter and exit the interconnection opening. Not all knots, but most knots have dominant registry errors. It should be noted that although the errors are accumulated, as shown in the expansion data FIG. Finally, there is a system error due to the uncertainty of the distance to HH211, but it can be ignored compared to other errors.
The reduction data of Nircam and NIRSPEC is available if there is a request from the corresponding author. The reduction data of the standard pipeline will be published in the Mast portal (https://mast. stsci. edu/portal/mashup/clients/mast/portal. html) one year after the observation date. There are two main causes of the errors in the unique movement. The first is the accuracy of the registered image between ESO VLT and JWST images, and is converted from the error of the arc second to the equivalent speed of the KM S-1. The same value is used for all unique movements. Other errors are determined by the mutual association by changing the input parameters such as the size of the box and seeing how much the measured exercise changes. In some knots, the error is small because the knots are beautiful and symmetrical, but in other knots, the error increases due to the confusion with other structures that enter and exit the interconnection opening. Not all knots, but most knots have dominant registry errors. It should be noted that although the errors are accumulated, as shown in the expansion data FIG. Finally, there is a system error due to the uncertainty of the distance to HH211, but it can be ignored compared to other errors.
The reduction data of Nircam and NIRSPEC is available if there is a request from the corresponding author. The reduction data of the standard pipeline will be published in the Mast portal (https://mast. stsci. edu/portal/mashup/clients/mast/portal. html) one year after the observation date.
Using the JWST Calibration Pipeline V. 1. 7. 2 (Reference 31), the V. 11. 16. 10 of the calibration reference data system (CRDS) and the CRDS context version 'jwst_0988. pmap' is used to use each. Raw data was reprocessed. The pipeline code has been published as a GitHub repository (https://github. com/spacetelescope/jwst), and the detailed documents on the installation, execution of the pipeline, and the settings for CRDS. INE . readedocs. io/en/latest/. The ROEBA tool was used to reduce the 1/f noise of Nircam data. The effects and corrections are described in ref. 32, and the code and usage are published in https://tshirt. Readedocs. io/en/latest/specific_modules/roeba. html. The masking of the expansion emission was combined with the Astropy 36 IO. FITS module and the ASTROPY Regions package 37. These two modules have the details of installation and usage on https://www. astropy. org/ and https://astropy-regions. Readthedocs. io/en/stable/. In order to correct the su b-pixel offset between the mosaics of the NIRCAM filter, the IO. Fits module was used for the analysis and editing of the file, and the Centroids. centroid_2dg module of Photutils was used for Centroid measurement. The latter is open to the public and has a detailed explanation about installation and use in https: //photutils. Readthedocs. io/en/stable/index. html. The visualization of the image was performed using Saoimage DS9 39.
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