text:
Anita Dongre is all for slow, relevant fashion
Sweety Kumari
Launching her first flagship store in Hyderabad, designer Anita Dongre says the pandemic has made people celebrate classy, timeless styles
Digital is a pragmatic route to take during the pandemic, even for luxury labels. The fashion world had always believed that prêt could be sold online but couture, which necessitates a personalised approach, is best done in person. Now, even that segment is exploring newer methods; video consultations, for instance, to keep the business afloat. However, with the subsequent 'Unlock's and the festive-wedding season bringing cheer to the fashion and textile sector, designer Anita Dongre took the leap of faith and launched her first flagship store in Hyderabad recently, confident of patronage from the city's splurge-happy clientele with deep pockets.
The initial plan was to open in summer and 50% of the work had been completed by mid-March. Resuming work in October, the store opened in time for the festive and wedding season. Clients can visit by appointment, complying with COVID-19 safety norms. As Anita puts it, "Buying luxury is a sensory experience unmatched by the internet despite our every effort to create a seamless extension."
Art meets architecture
Designed by architect Shonan Purie Trehan of Labwerk, the three-storey store spread over 4,000 square feet reflects Anita's fondness for Rajasthani art and architecture. "This was a rundown structure and it's been a pleasure to transform it into a home where art, fashion and emotion live. The façade is inspired by the stepwells of Rajasthan, and the interiors are filled with things that inspire me every day — Pichhwai paintings with scenes from nature, stone, marble and antique artwork," explains Anita.
A 50-year-old vintage ensemble worn by Pashtun women in the region bordering Afghanistan greets visitors at the entrance. The multi-coloured beads, threads and tassels narrate stories of embroidery traditions in the desert land. Anita emphasises that celebration of craftsmanship has been the core of her work, be it couture for men and women, the sustainable prêt line Grassroot, or her jewellery line Pink City.
As weddings became smaller and intimate, Anita launched her collection 'Love Song 2020', which she terms as an ode to the close-knit family celebrations during her childhood days. Launching this collection during the pandemic was sheer coincidence, she shares: "We conceptualised Love Song pre-lockdown, in a world that now feels so far away. It's been a relevant collection."
Dhaaga, the capsule collection that is hand embroidered by the women of SEWA (Self Employed Women's Association) and the designer's signature ensembles with gota patti work also continue to be relevant.
Though there has been a dent in sale volumes across designer labels, Anita looks at the silver lining — of fashion becoming personal, and classic styles being celebrated: "To be honest, this has always been my aesthetic — fuss-free, elegant and timeless," she says, taking pride in her ensembles standing the test of time.
When the pandemic set in, there was an increase in conversation about sustainable lifestyles and buying handmade, handcrafted ensembles. Anita is eager to gauge how long this approach will last: "Defining who benefits from every rupee spent has come into the spotlight. I hope more people adopt this approach with continued messaging to support local [crafts and artisans]," she says.
In June, Anita Dongre Foundation trained artisans in the rural clusters of Charoti and Dhanaveri in Maharastra to manufacture masks for distribution in rural areas and to COVID-19 frontline workers. "I have always believed in using design for good and fashion to empower. My commitment to that truth has only grown stronger in this hour of need," she says.
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redpajama_set_name: RedPajamaCommonCrawl


Filled with highs and lows for the Medical Center, 2017 was a year to remember. Here's a look back at the stories that made the year special. Thank you to everyone who contributed to UMMC's success stories.
Since the passage of the Health Care Collaboration Act of 2017 gave the Medical Center more flexibility in its clinical procurement processes, UMMC is projected to save more than $2.6 million in Fiscal Year 2018. These savings come at a critical time for the institution.
In his new book Desperate Surgery in the Pacific War: Doctors and Damage Control for American Wounded, 1941-45, Dr. Thomas Helling pays tribute to the brave physicians who, in the worst of circumstances, saved lives of soldiers who suffered unimaginable traumatic injuries. Helling gives voice to the true stories of courage and resourcefulness that need to be told.


text:
package test.hello.suribot.communication.ai;

import static org.junit.Assert.*;

import org.json.JSONObject;
import org.junit.Test;

import ai.api.AIServiceException;
import hello.suribot.communication.ai.AiController;
import hello.suribot.utils.EnvVar;

public class AiControllerTest {

	@Test
	public void sendMessagedTest(){
		AiController controller = new AiController();
		assertFalse(controller.sendMessage(null, null, null, null));
	}

	@Test
	public void callApiAiTest() {
		AiController controller = new AiController();
		try {
			controller.callApiAi(null, null, null);
		} catch (IllegalArgumentException | AIServiceException e) {
			assertTrue(true);
		}
		try {
			controller.callApiAi("message", EnvVar.TOKENAPIAI.getValue(), "fr");
		} catch (AIServiceException e) {
			assertTrue(true);
		}
	}

	@Test
	public void callRecastTest() {
		AiController controller = new AiController();
		assertEquals(controller.callRecast(null, null, null).toString(), new JSONObject().toString());
		assertEquals(controller.callRecast("", EnvVar.TOKENRECAST.getValue(), "fr").toString(), new JSONObject().toString());
		assertNotEquals(controller.callRecast("message", EnvVar.TOKENRECAST.getValue().toString(), "fr"), new JSONObject().toString());
	}

}

redpajama_set_name: RedPajamaGithub


text:
"If you happen to come upon a bird's nest along the way, in any tree or on the ground, with young ones or eggs, and the mother sitting on the young or on the eggs, you shall not take the mother with the young; you shall certainly let the mother go, but the young you may take for yourself, in order that it may be well with you and that you may prolong your days. Share Your Faith Products
The word that came to Jeremiah from the Lord: "Arise, and go down to the potter's house, and there I will let you hear my words." So I went down to the potter's house, and there he was working at his wheel. And the vessel he was making of clay was spoiled in the potter's hand, and he reworked it into another vessel, as it seemed good to the potter to do. Then the word of the Lord came to me: ... Christian Gifts
The son of a woman of the daughters of Dan, and his father was a man of Tyre. He is trained to work in gold, silver, bronze, iron, stone, and wood, and in purple, blue, and crimson fabrics and fine linen, and to do all sorts of engraving and execute any design that may be assigned him, with your craftsmen, the craftsmen of my lord, David your father.
"The house which I am about to build will be great, for greater is our God than all the gods. "But who is able to build a house for Him, for the heavens and the highest heavens cannot contain Him? So who am I, that I should build a house for Him, except to burn incense before Him? "Now send me a skilled man to work in gold, silver, brass and iron, and in purple, crimson and violet fabrics, and who knows how to make engravings, to work with the skilled men whom I have in Judah and Jerusalem, whom David my father provided. Christian Gifts
Much of the art surviving from Europe after the fall of the Western Roman Empire is Christian art, although this in large part because the continuity of church ownership has preserved church art better than secular works. While the Western Roman Empire's political structure essentially collapsed after the fall of Rome, its religious hierarchy, what is today the modern-day Roman Catholic Church commissioned and funded production of religious art imagery. Share Your Faith Products
Now King Solomon sent and brought Hiram from Tyre. He was a widow's son from the tribe of Naphtali, and his father was a man of Tyre, a worker in bronze; and he was filled with wisdom and understanding and skill for doing any work in bronze So he came to King Solomon and performed all his work. He fashioned the two pillars of bronze; eighteen cubits was the height of one pillar, and a line of twelve cubits measured the circumference of both. read more.
Now King Solomon sent and brought Hiram from Tyre. He was a widow's son from the tribe of Naphtali, and his father was a man of Tyre, a worker in bronze; and he was filled with wisdom and understanding and skill for doing any work in bronze So he came to King Solomon and performed all his work. He fashioned the two pillars of bronze; eighteen cubits was the height of one pillar, and a line of twelve cubits measured the circumference of both. read more. Christian Canvas Art
"Bezalel and Oholiab and every craftsman in whom the Lord has put skill and intelligence to know how to do any work in the construction of the sanctuary shall work in accordance with all that the Lord has commanded." And Moses called Bezalel and Oholiab and every craftsman in whose mind the Lord had put skill, everyone whose heart stirred him up to come to do the work. And they received from Moses all the contribution that the people of Israel had brought for doing the work on the sanctuary. They still kept bringing him freewill offerings every morning, so that all the craftsmen who were doing every sort of task on the sanctuary came, each from the task that he was doing, and said to Moses, "The people bring much more than enough for doing the work that the Lord has commanded us to do." ...
It was carved with cherubim and palm trees; and a palm tree was between cherub and cherub, and every cherub had two faces, a man's face toward the palm tree on one side and a young lion's face toward the palm tree on the other side; they were carved on all the house all around. From the ground to above the entrance cherubim and palm trees were carved, as well as on the wall of the nave. The doorposts of the nave were square; as for the front of the sanctuary, the appearance of one doorpost was like that of the other. The altar was of wood, three cubits high and its length two cubits; its corners, its base and its sides were of wood And he said to me, "This is the table that is before the LORD." The nave and the sanctuary each had a double door. Each of the doors had two leaves, two swinging leaves; two leaves for one door and two leaves for the other. Also there were carved on them, on the doors of the nave, cherubim and palm trees like those carved on the walls; and there was a threshold of wood on the front of the porch outside. There were latticed windows and palm trees on one side and on the other, on the sides of the porch; thus were the side chambers of the house and the thresholds. Bible Verse Wall Art
He made an altar of bronze, twenty cubits long and twenty cubits wide and ten cubits high. Then he made the sea of cast metal. It was round, ten cubits from brim to brim, and five cubits high, and a line of thirty cubits measured its circumference. Under it were figures of gourds, for ten cubits, compassing the sea all around. The gourds were in two rows, cast with it when it was cast. It stood on twelve oxen, three facing north, three facing west, three facing south, and three facing east. The sea was set on them, and all their rear parts were inward. Its thickness was a handbreadth. And its brim was made like the brim of a cup, like the flower of a lily. It held 3,000 baths. ... Share Your Faith Products
Then Moses said to the people of Israel, "See, the Lord has called by name Bezalel the son of Uri, son of Hur, of the tribe of Judah; and he has filled him with the Spirit of God, with skill, with intelligence, with knowledge, and with all craftsmanship, to devise artistic designs, to work in gold and silver and bronze, in cutting stones for setting, and in carving wood, for work in every skilled craft. And he has inspired him to teach, both him and Oholiab the son of Ahisamach of the tribe of Dan. ...
For the last 5 years, the in-house design team at the Faithlife Corporation has illustrated one Bible verse every day. This art has found its way onto t-shirts, magnets, and postcards—and now, a beautiful picture book. In print for the first time, art from Faithlife's Verse of the Day series paired with uplifting devotionals will encourage and inspire you. Share Your Faith Products
"You shall take two onyx stones and engrave on them the names of the sons of Israel, six of their names on the one stone and the names of the remaining six on the other stone, according to their birth. "As a jeweler engraves a signet, you shall engrave the two stones according to the names of the sons of Israel; you shall set them in filigree settings of gold.read more. Christian Gifts
"If you happen to come upon a bird's nest along the way, in any tree or on the ground, with young ones or eggs, and the mother sitting on the young or on the eggs, you shall not take the mother with the young; you shall certainly let the mother go, but the young you may take for yourself, in order that it may be well with you and that you may prolong your days. Christian Canvas Art
He measured the length of the building along the front of the separate area behind it, with a gallery on each side, a hundred cubits; he also measured the inner nave and the porches of the court. The thresholds, the latticed windows and the galleries round about their three stories, opposite the threshold, were paneled with wood all around, and from the ground to the windows (but the windows were covered), over the entrance, and to the inner house, and on the outside, and on all the wall all around inside and outside, by measurement.read more.
The Orthodox Church of Constantinople, which enjoyed greater stability within the surviving Eastern Empire was key in commissioning imagery there and glorifying Christianity. As a stable Western European society emerged during the Middle Ages, the Catholic Church led the way in terms of art, using its resources to commission paintings and sculptures. Share Your Faith Products
Every home is so much more than just walls and windows. Home is the place where we live, laugh, and love. It's an expression of who we are and what we believe. That's why we are committed to providing beautiful Christian art and inspirational home décor. Our passion is helping you create a place that reflects your faith and enables you to share it with others. So discover new ways to share your heart and God's love today! Christian Canvas Art
He made 300 shields of beaten gold, using three minas of gold on each shield, and the king put them in the house of the forest of Lebanon. Moreover, the king made a great throne of ivory and overlaid it with refined gold. There were six steps to the throne and a round top to the throne at its rear, and arms on each side of the seat, and two lions standing beside the arms. Twelve lions were standing there on the six steps on the one side and on the other; nothing like it was made for any other kingdom. All King Solomon's drinking vessels were of gold, and all the vessels of the house of the forest of Lebanon were of pure gold. None was of silver; it was not considered valuable in the days of Solomon. Bible Verse Wall Art
The Orthodox Church of Constantinople, which enjoyed greater stability within the surviving Eastern Empire was key in commissioning imagery there and glorifying Christianity. As a stable Western European society emerged during the Middle Ages, the Catholic Church led the way in terms of art, using its resources to commission paintings and sculptures.
19 designers and 31 writers invested their energy and creativity to this collection, each riffing on the timeless, inspired words of Scripture. Each designer worked hard to capture the essence of each verse in its historical and cultural context, and to design in a way that makes clear the way in which the original readers would have understood it. Then, after each design was complete, a writer reflected on each piece of art and the verse that inspired it. The result is 100 pairs of art and devotional that illuminate the words of Scripture. Share Your Faith Products
Until the adoption of Christianity by Constantine Christian art derived its style and much of its iconography from popular Roman art, but from this point grand Christian buildings built under imperial patronage brought a need for Christian versions of Roman elite and official art, of which mosaics in churches in Rome are the most prominent surviving examples. Christian art was caught up in, but did not originate, the shift in style from the classical tradition inherited from Ancient Greek art to a less realist and otherworldly hieratic style, the start of gothic art. Christian Canvas Art
This is the book of the generations of Adam. When God created man, he made him in the likeness of God. Male and female he created them, and he blessed them and named them Man when they were created. When Adam had lived 130 years, he fathered a son in his own likeness, after his image, and named him Seth. The days of Adam after he fathered Seth were 800 years; and he had other sons and daughters. Thus all the days that Adam lived were 930 years, and he died. ... Christian Canvas Art
"You shall take two onyx stones and engrave on them the names of the sons of Israel, six of their names on the one stone and the names of the remaining six on the other stone, according to their birth. "As a jeweler engraves a signet, you shall engrave the two stones according to the names of the sons of Israel; you shall set them in filigree settings of gold.read more. Christian Canvas Art
King Solomon was king over all Israel, and these were his high officials: Azariah the son of Zadok was the priest; Elihoreph and Ahijah the sons of Shisha were secretaries; Jehoshaphat the son of Ahilud was recorder; Benaiah the son of Jehoiada was in command of the army; Zadok and Abiathar were priests; Azariah the son of Nathan was over the officers; Zabud the son of Nathan was priest and king's friend; ...
In the four hundred and eightieth year after the people of Israel came out of the land of Egypt, in the fourth year of Solomon's reign over Israel, in the month of Ziv, which is the second month, he began to build the house of the Lord. The house that King Solomon built for the Lord was sixty cubits long, twenty cubits wide, and thirty cubits high. The vestibule in front of the nave of the house was twenty cubits long, equal to the width of the house, and ten cubits deep in front of the house. And he made for the house windows with recessed frames. He also built a structure against the wall of the house, running around the walls of the house, both the nave and the inner sanctuary. And he made side chambers all around. ... Christian Canvas Art
The Lord said to Moses, "See, I have called by name Bezalel the son of Uri, son of Hur, of the tribe of Judah, and I have filled him with the Spirit of God, with ability and intelligence, with knowledge and all craftsmanship, to devise artistic designs, to work in gold, silver, and bronze, in cutting stones for setting, and in carving wood, to work in every craft. ... Share Your Faith Products
"You shall make an altar on which to burn incense; you shall make it of acacia wood. A cubit shall be its length, and a cubit its breadth. It shall be square, and two cubits shall be its height. Its horns shall be of one piece with it. You shall overlay it with pure gold, its top and around its sides and its horns. And you shall make a molding of gold around it. And you shall make two golden rings for it. Under its molding on two opposite sides of it you shall make them, and they shall be holders for poles with which to carry it. You shall make the poles of acacia wood and overlay them with gold. ... Bible Verse Wall Art
And it will come about in that day, that every place where there used to be a thousand vines, valued at a thousand shekels of silver, will become briars and thorns. People will come there with bows and arrows because all the land will be briars and thorns. As for all the hills which used to be cultivated with the hoe, you will not go there for fear of briars and thorns; but they will become a place for pasturing oxen and for sheep to trample. Christian Gifts
Comfort, comfort my people, says your God. Speak tenderly to Jerusalem, and cry to her that her warfare is ended, that her iniquity is pardoned, that she has received from the Lord's hand double for all her sins. A voice cries: "In the wilderness prepare the way of the Lord; make straight in the desert a highway for our God. Every valley shall be lifted up, and every mountain and hill be made low; the uneven ground shall become level, and the rough places a plain. And the glory of the Lord shall be revealed, and all flesh shall see it together, for the mouth of the Lord has spoken." ...
1 Then the LORD said to Moses, 2 "See, I have chosen Bezalel son of Uri, the son of Hur, of the tribe of Judah, 3 and I have filled him with the Spirit of God, with wisdom, with understanding, with knowledge and with all kinds of skills— 4 to make artistic designs for work in gold, silver and bronze, 5 to cut and set stones, to work in wood, and to engage in all kinds of crafts. 6 Moreover, I have appointed Oholiab son of Ahisamak, of the tribe of Dan, to help him. Also I have given ability to all the skilled workers to make everything I have commanded you: Bible Verse Wall Art
He made 300 shields of beaten gold, using three minas of gold on each shield, and the king put them in the house of the forest of Lebanon. Moreover, the king made a great throne of ivory and overlaid it with refined gold. There were six steps to the throne and a round top to the throne at its rear, and arms on each side of the seat, and two lions standing beside the arms. Twelve lions were standing there on the six steps on the one side and on the other; nothing like it was made for any other kingdom. All King Solomon's drinking vessels were of gold, and all the vessels of the house of the forest of Lebanon were of pure gold. None was of silver; it was not considered valuable in the days of Solomon. Share Your Faith Products
"You saw, O king, and behold, a great image. This image, mighty and of exceeding brightness, stood before you, and its appearance was frightening. The head of this image was of fine gold, its chest and arms of silver, its middle and thighs of bronze, its legs of iron, its feet partly of iron and partly of clay. As you looked, a stone was cut out by no human hand, and it struck the image on its feet of iron and clay, and broke them in pieces. Then the iron, the clay, the bronze, the silver, and the gold, all together were broken in pieces, and became like the chaff of the summer threshing floors; and the wind carried them away, so that not a trace of them could be found. But the stone that struck the image became a great mountain and filled the whole earth.
Much of the art surviving from Europe after the fall of the Western Roman Empire is Christian art, although this in large part because the continuity of church ownership has preserved church art better than secular works. While the Western Roman Empire's political structure essentially collapsed after the fall of Rome, its religious hierarchy, what is today the modern-day Roman Catholic Church commissioned and funded production of religious art imagery. Christian Gifts
"Come, everyone who thirsts, come to the waters; and he who has no money, come, buy and eat! Come, buy wine and milk without money and without price. Why do you spend your money for that which is not bread, and your labor for that which does not satisfy? Listen diligently to me, and eat what is good, and delight yourselves in rich food. Incline your ear, and come to me; hear, that your soul may live; and I will make with you an everlasting covenant, my steadfast, sure love for David. Behold, I made him a witness to the peoples, a leader and commander for the peoples. Behold, you shall call a nation that you do not know, and a nation that did not know you shall run to you, because of the Lord your God, and of the Holy One of Israel, for he has glorified you. ... Christian Canvas Art
Love is patient and kind; love does not envy or boast; it is not arrogant or rude. It does not insist on its own way; it is not irritable or resentful; it does not rejoice at wrongdoing, but rejoices with the truth. Love bears all things, believes all things, hopes all things, endures all things. Love never ends. As for prophecies, they will pass away; as for tongues, they will cease; as for knowledge, it will pass away. Bible Verse Wall Art
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text:
\section{Introduction}

The determination of the magnetic topology of sunspots has been an important topic in solar physics during the last decades. A global scale picture has emerged, showing that sunspots are formed by a flux tube with a strong and vertical magnetic field at the axis, in the umbral center, which becomes weaker and more horizontal at radial distances farther from the flux tube's axis \citep[\rmit{e.g.},][]{Tiwari+etal2015}. The improvement in the resolution of the observations has revealed a more complex picture, where fine structure is present in the umbra and penumbra of sunspots \citep[see][for a review]{Solanki2003, Borrero+Ichimoto2011}. The magnetic structure is a result of the close interplay between plasma motions and magnetic fields, and it is subject to significant changes during the evolution of the sunspot.

\begin{figure*}[!ht]
 \centering
 \includegraphics[width=14cm]{Stokes_IV_deconv.eps}
  \caption{Stokes I (top panel) and Stokes V (bottom panel) at position C on Fig. \ref{fig:mapa_GREGOR} normalized to quiet Sun continuum intensity.}
  \label{fig:spectra}
\end{figure*}

The decay of a sunspot is a slow process, which usually takes place over several days. The mechanisms leading to the disappearance of the sunspot's magnetic flux are still not fully understood and remain one of the most challenging problems of sunspot physics. Most sunspots exhibit a large-scale outflow called ``moat flow'' \citep{Meyer+etal1974} beyond their visible outline, whose physical origin differs from that of the Evershed flow \citep{Lohner-Bottcher+Schlichenmaier2013}. It was first detected spectroscopically \citep{Sheeley1972} and then by tracking Moving Magnetic Features \citep[MMFs,][]{Harvey+Harvey1973}. MMFs with the same polarity as the umbra have been associated with sunspot decay \citep[\rmit{e.g.},][]{MartinezPillet2002} because they extract net flux from the spot \citep{Zhang+etal1992}. They disperse this flux, which is then removed from the photosphere. However, the flux removal mechanism remains elusive. MMFs move through the moat flow, accumulating at the edge of the moat region. On the other hand, pairs of MMFs with opposite polarities do not contribute to the flux removal since they do not carry net flux. \citet{Deng+etal2007} studied the flow field in a decaying sunspot and concluded that the mechanisms contributing to the decay are the fragmentation of the umbra, cancellation of MMFs that encounter opposite polarity areas at the moat's outer boundary, and flux transport by MMFs to regions with the same polarity as the sunspot. After the disappearance of the sunspot, the flow pattern in that location exhibits significant differences with flows at other quiet Sun regions \citep{Verma+etal2012}. \citet{BellotRubio+etal2008} studied the decay of a penumbra using spectropolarimetric data. Blue-shifted finger-like structures of weak and horizontal magnetic field extending outward from the border of the umbra were identified. They proposed that these structures are penumbral field lines that rise to the chromosphere and contribute to the disappearance of the penumbra at photospheric levels.

Sunspot light bridges can be formed due to the fragmentation of the umbra in the decay phase or during the merging of different magnetized areas during the formation of the sunspot in complex active regions \citep{Bray+Loughhead1964, GarciadelaRosa1987}. At the last stages of a sunspot, as a consequence of the splitting of the umbra the photospheric-like conditions are recovered, and a granulation pattern similar to the quiet Sun is found in light bridges \citep{Vazquez1973}, although the light bridge convection cells do differ significantly from normal granules \citep{Lagg+etal2014}. Understanding the decay of sunspots requires the study of the magnetic and dynamical structure of light bridges. Previous studies have classified light bridges based on their morphological properties. Light bridges separating two umbral regions are called ``strong light bridges'' \citep[\rmit{e.g.},][]{Sobotka+etal1993, Sobotka+etal1994,Jurcak+etal2006, Rimmele2008}. Their brightness is similar to that of the penumbra and they usually appear between two regions with the same polarity. ``Faint light bridges'' \citep[\rmit{e.g.}][]{Lites+etal1991, Sobotka+etal1993} are elongated bright structures which penetrate the umbra. They are composed of rows of bright grains with sizes comparable to umbral dots. Light bridges can exhibit different internal structure. Most of them show several segments along their length that resemble granules \citep{Berger+Berdyugina2003}, while some light bridges are similar to the bright filaments seen in the penumbra \citep{Lites+etal2004}. All types show a weakened magnetic field strength relative to the surrounding umbra and more inclined field lines \citep[\rmit{e.g.}][]{Beckers+Schroter1969, Lites+etal1991, Leka1997}, which in some case even exhibit a polarity reversal \citep{Lagg+etal2014}. Observations are consistent with a reduced field strength in the photosphere with a magnetic canopy extending from both sides of the light bridge and merging at the top \citep{Jurcak+etal2006, Lagg+etal2014}. The velocity field measured in light bridges shows evidence of their convective origin \citep{Rimmele1997, Hirzberger+etal2002, Lagg+etal2014}. Recently, \citet{Schlichenmaier+etal2016} have also found evidence that the umbral magnetic field wraps around light bridges. They defined a new type, the plateau light bridge, with `Y' shaped dark canals that resemble penumbral grains and suggest the presence of inclined magnetic fields. Several dynamic phenomena have been detected at the chromosphere above light bridges, including recurrent plasma ejections visible in H$\alpha$ \citep{Roy1973,Asai+etal2001}, \CaIIH\ \citep{Shimizu+etal2009} and other bands \citep[AIA 1600 and 1700 \AA, IRIS 1330 and 1400 \AA,][]{Toriumi+etal2015}, brightness enhancements in TRACE 1600 \AA\ band \citep{Berger+Berdyugina2003}, or fan-shaped jets observed in H$\alpha$ \citep{Robustini+etal2016}. All these processes are considered to be caused by the interaction of the light bridge magnetic field with the surrounding atmosphere through magnetic reconnection events.

Sunspot evolution is driven by the interaction of magnetic fields and plasma. The relevance of the plasma motions in the molding of the magnetic field is quantified by the plasma-$\beta$ parameter \citep[\rmit{e.g.},][]{Gary2001}. It is defined as the ratio between the gas pressure, $P_\mathrm{g}$, and the magnetic pressure, $P_\mathrm{m}$, \rmit{i.e.}, $\beta=P_\mathrm{g}/P_\mathrm{m}=2\mu_0P_\mathrm{g}/B^2$, where $\mu_0$ is the magnetic permeability and $B$ is the magnetic field strength. In those regions where $\beta\gg 1$ the plasma dominates over the magnetic field, which can be bent and dragged following plasma motions. On the other hand, where $\beta\ll 1$ the magnetic field is not influenced by the plasma, and motions can only occur along field lines. In these regions the magnetic field acquires a force-free configuration \citep[see Sect. 2.4 from][]{Borrero+Ichimoto2011}. In sunspot atmospheres, the umbra shows small $\beta$ values ($\beta <1$) at the low photosphere and higher values ($\beta >1$) as we move towards the edges of the spot \citep[\rmit{i.e.},][]{Mathew+etal2004}, although for at least one other sunspot, plasma  $\beta>1$ everywhere in the sunspot's lower atmosphere \citep{Solanki+etal1993}. At higher layers the atmosphere is dominated by the magnetic field ($\beta\ll 1$).

In this study, we aim at analyzing the thermodynamic and magnetic structure of a sunspot during its decay, a few days before it completely disappeared. We concentrate on the deep photosphere, where the magnetic field configuration is more dependent on the plasma dynamics. In Sect. \ref{sect:observations}, we present the data set and qualitatively describe the evolution of the active region during its disk passage. Section \ref{sect:inversion} shows the inversion techniques used in the analysis, and the results are described in Sect. \ref{sect:results}. Finally, conclusions are outlined in Sect. \ref{sect:conclusions}.

\section{Observations}
\label{sect:observations}
Spectropolarimetric data of the active region NOAA 12096 were obtained on 2014 June 27 from 8:28 to 9:13 UT with the 1.5-meter GREGOR solar telescope \citep{Schmidt+etal2012} at the Observatorio del Teide, Tenerife, Spain. The center of the analyzed region was located at the solar position $x=-184''$, $y=100''$, which corresponds to heliocentric angle of $\Theta =12.4^o$ ($\mu=\cos\Theta=0.98$).

The full data set consists on 10 maps of the four Stokes parameters, each of them covering a scanned area of $61''\times 7.8''$, acquired with the GREGOR Infrared Spectrograph \citep[GRIS,][]{Collados+etal2012}. The pixel size along the slit was 0.135\hbox{$^{\prime\prime}$}. For the construction of the maps, 60 consecutive slit positions were included by shifting the slit in increments of 0.135\hbox{$^{\prime\prime}$}. The number of accumulations per recording was 10 with an integration time of 40 ms each. A full map was completed in 4.5 min. The wavelength scale was calibrated on an absolute scale \citep{MartinezPillet+etal1997}, correcting for several systematic effects such as Earth's orbital motions and the solar gravitational redshift \citep[see Appendices A and B of][]{Kuckein+etal2012b}. The spectral range spans from 10823.73 to 10842.01 \AA\ with a spectral sampling of 18.1 m\AA\ pixel$^{-1}$. Figure \ref{fig:spectra} shows the Stokes $I$ and $V$ parameters at location C near the umbra/penumbra boundary (see Fig. \ref{fig:mapa_GREGOR}). The spectral range of the spectropolarimeter comprises several spectral lines of interest, such as the photospheric \mbox{Si\,\specchar{i}}\ 10827 \AA\ and \mbox{Ca\,\specchar{i}}\ 10839 \AA\ lines and the chromospheric \mbox{He\,\specchar{i}}\ 10830 \AA\ triplet. In this study we focus on the analysis of the two aforementioned photospheric lines.

Standard procedures for dark and flat-field correction and polarimetric calibration \citep{Collados1999, Collados2003} were applied to all images. The telescope calibration unit \citep{Hofmann+etal2012} was used for the polarimetric calibration. The GREGOR Adaptative Optics System \citep[GAOS,][]{Berkefeld+etal2012} was locked on nearby structures, improving substantially the image quality. GREGOR's altitude-azimuthal mount introduced an image rotation \citep{Volkmer+etal2012}. Obtaining co-spatial maps required the application of some correction to compensate this rotation, which amounts to $11^\circ$ during the whole period of the observations. However, since the maps do not show significant evolution during the observed 45 min, we have decided to focus the analysis on each individual map so that a temporal series of co-spatial maps is not necessary. The image rotation during the acquisition of each map (slightly higher than $1^\circ$) has been neglected.

\begin{figure*}[!ht]
 \centering
 \includegraphics[width=16cm]{evolution_HMI.eps}
  \caption{HMI continuum images of the evolution of the active region NOAA 12096 between 2014 June 24\,--\,30. Date and time of the images are indicated at the top of each panel. The tilted rectangle in the bottom left panel indicates the FOV covered by the GRIS observations.}
  \label{fig:evolution_HMI}
\end{figure*}

\subsection{PSF and stray light corrections}
\label{sect:PSF}

The spatial resolution of solar ground-based observations is limited by the turbulence in the Earth atmosphere and by the optical properties of the telescope \citep[\rmit{e.g.},][]{MartinezPillet1992, Chae+etal1998, WedemeyerBohm2008}. The distortion that these effects produce on the observations is characterized by the Point Spread Function (PSF), whose contributions are commonly approximated by analytical functions. The PSFs are usually dominated by an Airy pattern and, as a consequence of its tails, light observed at the focal plane is contaminated by light coming from distant spatial locations. This spurious light is known as "stray light". Deconvolution techniques are a common approach for correcting this effect. In the case of two dimensional observations (broad-band imaging or narrow-band spectroscopy) an effective instantaneous PSF can be estimated observationally \citep[\rmit{e.g.},][]{vonderLuhe1993, vanNoort+etal2005}. These techniques are not applicable to maps obtained from the scanning of adjacent spatial steps using a slit-spectrograph, since at each scan the PSF includes contributions from surrounding regions not covered by the one-dimensional slit. Instead, the deconvolution scheme is applied to each monochromatic map using a static PSF \citep[\rmit{e.g.}][]{Beck+etal2011,QuinteroNoda+etal2015}. The correction for stray light using deconvolution techniques has produced observations with unprecedented spatial resolution and has allowed the study of the Sun at finer scales \citep[\rmit{e.g.},][]{Scharmer+etal2011, Joshi+etal2011, Henriques2012}.

\citet{Schlichenmaier+Franz2013} have claimed that the correction for scattered light can produce artifacts on the velocity measurements if the PSF of the stray light is not well characterized. In this work, we have empirically determined the PSF of the GRIS instrument from observations of the Mercury transit in front of the Sun on 2016 May 9. During the observations, weather conditions were not optimum, with some clouds at the level of the observatory. A wavelength-integrated map of Mercury transiting the solar disk was obtained in the 1.56 $\mu$m region using GRIS polarimetric mode. The scan was composed of 300 consecutive recordings with a 0.135\hbox{$^{\prime\prime}$}\ step size. The integration time per individual image was 100 ms and the number of accumulations was 3.

A synthetic circular image simulating the undegraded Mercury covering a homogeneous solar surface was created and convolved with a PSF profile given by

\begin{equation}
\phi (r)=\alpha G_1(r,\sigma_1)+(1-\alpha)G_2(r,\sigma_2),
\label{eq:PSF}
\end{equation}

\noindent where $G_1$ and $G_2$ are two Gaussians with the rms widths given by $\sigma_1$ and $\sigma_2$, respectively. The first Gaussian represents the spatial resolution of the telescope (including the seeing) and the second Gaussian accounts for the instrumental stray light. The parameter $\alpha$ is the relative contribution of each Gaussian. The parameters $\alpha$, $\sigma_1$, and $\sigma_2$ were obtained from a non-linear fit of the synthetic convolved circular image to the observed Mercury map.

The fit yields $\alpha=0.584\pm0.001$, $\sigma_1=1.385\pm0.001$\hbox{$^{\prime\prime}$}, and $\sigma_2=5.030\pm0.001$\hbox{$^{\prime\prime}$}. The FWHM of the first Gaussian (3.26\hbox{$^{\prime\prime}$} ) is consistent with the angular resolution of the observations, which were seeing-limited to 3.3\hbox{$^{\prime\prime}$}. This fact supports the assumption of the PSF proposed in Eq. \ref{eq:PSF} and allow us to reasonably argue that the second Gaussian gives the stray light contamination, with a FWHM of 11.8\hbox{$^{\prime\prime}$}\ and a relative weight of approximately 42\%.

The spectropolarimetric maps of the sunspot were deconvolved using a principal component analysis regularization \citep{RuizCobo+AsensioRamos2013}. We used a PSF given by Eq. \ref{eq:PSF}, but substituted $G_1(r,\sigma_1)$ by the Airy profile of the GREGOR telescope with the radius of the aperture corresponding to the Fried parameter $r_0$. During the scanning of the map analysed in this paper, the average value for the whole scan at 10830 \AA\ was $r_0=50.7$ cm. Due to the unfortunate seeing conditions during the Mercury transit, the small-scales properties of the stray light can be masked under the seeing contribution to the $G_1$ component of the PSF.

\subsection{Evolution of the sunspot}
\label{sect:evolution}

Continuum images obtained with the Helioseismic and Magnetic Imager \citep[HMI,][]{Schou+etal2012} on board the Solar Dynamic Observatory (SDO) have been examined in order to discuss the temporal evolution over a few days of the sunspot NOAA 12096 during its decay. HMI provides full disk observations with 4096$\times$4096 pixels and a pixel size of 0.5\hbox{$^{\prime\prime}$}. A selection of one image every 12 minutes between 2014 June 23 UT 16:00 and 2014 July 1 UT 23:48 was extracted from the HMI database. The full temporal series includes 1000 time steps.

Figure \ref{fig:evolution_HMI} shows a sample of six continuum images with a cadence of one day, except for the last panel, which corresponds to two days after the previous snapshot. A movie with the evolution of the sunspot during the time span indicated in the previous paragraph can be found in the online material. Between June 23 and June 26 the sunspot group was classified with a Hale class $\alpha$. During this time, part of the umbra separates from the center of the sunspot and moves towards the east. On June 26 at 08:48 UT, this region is completely detached from the outer penumbra of the sunspot. At the same time, a darker penumbral region (which appears as a dark pore-like structure at $x=-735$, $y=122.5$ on June 24 at 08:48 UT) moves towards the umbra. On June 27 this region is separated from the umbral core and from a ``spike-like'' extension of the main umbra by a zone with penumbral brightness. It forms the ``strong light bridge'' that is analysed in this study. Our GRIS observations were taken at that moment. The area covered by them is delineated by solid black lines in the bottom left panel of Fig. \ref{fig:evolution_HMI}. At this time, the group was classified as a $\beta$-region, although the region under investigation only shows negative polarity. The dark pore-like feature then merges with the rest of the umbra, forming an extended umbra with internal structure. At the last stages of the evolution of the sunspot, the umbra is divided by a light-bridge into two separated dark regions with the same polarity (see last panel of Fig. \ref{fig:evolution_HMI}), and finally it loses the surrounding penumbra. A C-class flare on June 24 at 20:56 UT was associated with this active region.

A section of the field-of-view (FOV) covered by the GRIS observations is shown in Fig. \ref{fig:mapa_GREGOR}. It corresponds to the continuum intensity at a wavelength close to the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line. This is the fifth map of the series acquired with GRIS and it was obtained between 08:46 and 08:50 UT. Since the ten maps of the series provide similar results, from this point onwards all figures and discussion refer to this time step. The contours overplotted on the map delimit the boundaries of some masks, which have been applied for the analysis of the data. The region inside the white line includes the darkest part of the umbra and in the following this mask will be referred as ``dark umbra''. What we term the ``faint umbra'' corresponds to the area between the white line and the black solid line and also the small umbra around $x=13''$ and $y=7''$. The ``penumbra'' is delimited by the black dashed and solid lines. Finally, the area surrounded by the dotted line between the dark pore-like feature and the umbra will be called ``light bridge''.

\begin{figure*}[!ht]
 \centering
 \includegraphics[width=14cm]{mapa_intensidad_deconv.eps}
  \caption{Continuum intensity map normalized to the average continuum intensity in the quiet Sun $\langle I^\mathrm{QS}_\mathrm{cont}\rangle$ obtained with GRIS on June 27 between 08:46 and 08:50 UT. Points $A$, $B$, and $C$ correspond to the locations used for Figs. \ref{fig:spectra}, \ref{fig:RFs}, \ref{fig:inversion_ff}, and \ref{fig:inversion_umbra}. The contour lines mark the boundaries of the masks used for the analysis in Sect. \ref{sect:results}: ``Dark umbra'' inside the white line, ``faint umbra'' delimited by the black solid line and the white line, ``penumbra'' between the black solid line and the dashed lines, and the ``light bridge'' inside the dotted line.}
  \label{fig:mapa_GREGOR}
\end{figure*}

\section{Spectral lines inversion and data analysis}
\label{sect:inversion}

The photospheric \mbox{Si\,\specchar{i}}\ 10827 \AA\ and \mbox{Ca\,\specchar{i}}\ 10839 \AA\ lines were inverted simultaneously using the ``Stokes Inversion based on Response functions'' (SIR) code \citep{RuizCobo+delToroIniesta1992}. SIR yields the thermal, dynamic, and magnetic depth-dependent stratification of the atmosphere that best matches the observed Stokes profiles. The solution is achieved after an iterative process, where the numerical integration of the radiative transfer equation is performed under the assumption of local thermodynamic equilibrium and using the spectral line response functions (RFs), which represent the partial derivatives of the Stokes parameters with respect to the various atmospheric parameters (at different depths).

The \mbox{Si\,\specchar{i}}\ 10827 \AA\ line has been used for probing the photosphere in many solar studies \citep[\rmit{e.g.},][]{Centeno+etal2006, Bloomfield+etal2007, Felipe+etal2010b, Kuckein+etal2012a}. Its proximity to the chromospheric \mbox{He\,\specchar{i}}\ 10830 \AA\ triplet makes this spectral region an ideal testing ground for simultaneous analysis of the photosphere and chromosphere. On the other hand, the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line, located a few {\AA}ngstr{\"o}m towards the red, has been widely overlooked \citep[though see][]{Joshi+etal2016, Balthasar+etal2016}. The broad spectral range of GRIS allows the simultaneous observation of all these spectral lines. The inclusion of the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line in the analysis rewards us with a better sampling of the deeper atmospheric layers, as can be seen in its response functions. Figure \ref{fig:RFs} shows the response functions of Stokes $I$ to the temperature and Stokes $V$ to the magnetic field strength for the \mbox{Si\,\specchar{i}}\ 10827 \AA\ and \mbox{Ca\,\specchar{i}}\ 10839 \AA\ lines at location $A$ in Fig. \ref{fig:mapa_GREGOR}. The top panels show that the \mbox{Si\,\specchar{i}}\ line is senstitive to heights up to $\log\tau=-3$, while the highest sensitivity of core of the \mbox{Ca\,\specchar{i}}\ line is slightly above the height of the continuum formation. The Stokes $V$ signal of the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line is sensitive to the magnetic field in a spectral range of 1 \AA\ centered at the core of the line. The maximum value of the RF at a specific wavelength is found at $\log\tau=-2.7$, where $\tau$ corresponds to the continuum optical depth at 5000~\AA. On the other hand, the peak of the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ RF is located at a larger optical depth, around $\log\tau=-0.4$. The aforementioned results refer to the RFs at location A. We have computed the RFs to magnetic field perturbations at several locations, including quiet Sun, penumbral, and umbral regions in order to retrieve an estimate of the average formation height of the \mbox{Ca\,\specchar{i}}\ and \mbox{Si\,\specchar{i}}\ lines. The analysis shows that their highest sensitivity to the magnetic field is found around $\log\tau=-0.5$ and $-2.2$, respectively. We estimate that the RFs of the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line are sufficiently high to retrieve reliable inversions of the data for $\log\tau$ lower than +0.3. The upper limit, where the atmospheric parameters obtained from the inversions are trustworthy, is given by the RFs of the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line. Thus, in the following, all the results derived from the simultaneous inversions of both lines will be restricted to the $\log\tau$ range between $+0.3$ and $-4.0$.

\begin{figure}[!ht]
 \centering
 \includegraphics[width=9cm]{RF_It_Vb_si_ca.eps}
  \caption{Normalized response functions of Stokes I to temperature (top panels) and Stokes V to the magnetic field strength (middle and bottom panels) for the atmosphere at location $A$. Top panels: response functions of Stokes I to temperature of the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line (left panel) and \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line (right panel). The region between the vertical while solid lines has been neglected for the inversions. Middle panels: response functions of Stokes V to magnetic field of the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line (left panel) and \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line (right panel). Bottom panels: variation of the response functions of Stokes V to magnetic field of the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line (dashed line) and the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line (dotted line) with $\log\tau$ at the wavelengths indicated by the dashed and dotted lines in the middle panels, respectively.}
  \label{fig:RFs}
\end{figure}

The SIR code requires an initial guess for the atmospheric model. We choose the cool umbral model from \citet{Collados+etal1994}, covering the optical depth range $+1.4\ge \log\tau\ge -5.0$. The temperature stratification $T(\tau)$ was inverted using five nodes, three nodes were used for magnetic field strength $B(\tau)$ and magnetic field inclination $\gamma(\tau)$, and two nodes for line-of-sight (LOS) velocity $v(\tau)$. The magnetic field azimuth $\chi$ was set to be independent with height, so that a constant azimuth was imposed in the initial model and only one node was selected for it.

The solar abundances were taken from \citet{Asplund+etal2009}, while the atomic data for the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line were obtained from \citet{Borrero+etal2003}. Since the core of the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line is formed in non-LTE conditions, a spectral region with a 0.2 \AA\ width centered at the peak of the line has been neglected for the inversions (see top left panel of Fig. \ref{fig:RFs}). This mask has only been applied to the intensity profile and the spectral region neglected has been chosen based on a comparison between a quiet Sun reference atmosphere \citep[HSRA,][]{Gingerich+etal1971} and the temperature stratification retrieved from inversions of the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line from the FTS atlas \citep{Kurucz+etal1984} with different masks. We have assumed that Stokes Q, U, and V are not affected by non-LTE conditions. The atomic parameters of the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line were determined semi-empirically. The line was synthesized iteratively in the HSRA atmosphere changing the values of the enhancement factor to the van der Waals coefficient $E$ and the logarithm of the multiplicity of the level times the oscillator strength $\log(gf)$. This procedure was repeated until an agreement with the observed intensity in the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line from the FTS atlas was achieved. For the abundances used in this study, we find $E=1.0$ and $\log(gf)=0.10$. The different values of the macroturbulence introduced in the HSRA model used for the synthesis can lead to the determination of different $E$ and $\log(gf)$ parameters. We set the macroturbulence to 1.7 km s$^{-1}$, since with this value and the atomic parameters of the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line from \citet{Borrero+etal2003}, the intensity profile of the \mbox{Si\,\specchar{i}}\ line synthesized in the HSRA model reproduces that from the FTS atlas.

Figures \ref{fig:inversion_ff} and \ref{fig:inversion_umbra} show a comparison between the observed Stokes profiles (thin line) and the results from the simultaneous inversion of the two photospheric lines (thick line) at two different positions. Each figure is composed of eight panels which represent the Stokes $I$, $Q$, $U$, and $V$ parameters for the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line (top panels) and the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line (bottom panels). Figure \ref{fig:inversion_ff} shows the profiles at a point in the light bridge. Its location is indicated with the letter $A$ in Fig. \ref{fig:mapa_GREGOR}. Figure \ref{fig:inversion_umbra} corresponds to the umbral atmosphere marked as $B$ in Fig. \ref{fig:mapa_GREGOR}. In both locations the SIR results show a satisfactory performance, providing an inferred atmosphere that captures the most relevant features present in the observed profiles. The continuum next to the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line is slightly below that from the observed profiles. Deep layer temperatures depending on this line might be a bit low. At the umbral position (Fig. \ref{fig:inversion_umbra}), the intensity absorption profile of the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line is decomposed into two $\sigma$-components with circular polarization, as can be seen in the Stokes $V$ profile. This fact points to a strong magnetic field in the direction of the LOS. According to the sign of the lobes in Stokes $V$, the polarity of the umbra is negative. On the other hand, at location A the magnetic field is not strong enough to produce a visible Zeeman splitting in the intensity of the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line. The reduction of the LOS magnetic field is also evident in the reduced wavelength shift of the Stokes $V$ lobes. Stokes $Q$ and $U$ show significant values, indicating the presence of a considerable horizontal magnetic field.

The determination of the magnetic field perpendicular to the LOS from the linear polarization signals (Stokes $Q$ and $U$) leads to two compatible solutions which differ by 180$^\circ$ in its azimuthal direction. Several techniques have been developed to resolve this ambiguity \citep[\rmit{e.g.},][]{Lites+etal1995, Leka+etal2009}. We have addressed this issue by assuming an approximately radial structure inside the sunspot and carefully chosen the azimuth origin around the center of the spot. The azimuth value retrieved from the inversion was changed by 180$^\circ$ in those regions where it was needed in order to satisfy this assumption.

\begin{figure*}[!ht]
 \centering
 \includegraphics[width=16cm]{inversion_si_ca_freefield_deconv.eps}
  \caption{Stokes parameters at location $A$ (light bridge) in Fig. \ref{fig:mapa_GREGOR} for the \mbox{Si\,\specchar{i}}\ 10827 \AA\ line (top panels) and the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line (bottom panel). Thin lines correspond to the observed profiles and thick lines to the fit obtained with SIR. The wavelength $\Delta\lambda=0$ refers to the line core. The physical parameters inferred from the inversion at $\log\tau=-0.5$ are $v=-0.01$ km s$^{-1}$, $B=568$ G, $\gamma=107^{\circ}$, and $\chi=240^{\circ}$, and at $\log\tau=-2.2$ are $v=-0.62$ km s$^{-1}$, $B=1339$ G, $\gamma=151^{\circ}$, and $\chi=190^{\circ}$.}
  \label{fig:inversion_ff}
\end{figure*}

\begin{figure*}[!ht]
 \centering
 \includegraphics[width=16cm]{inversion_si_ca_umbra_deconv.eps}
  \caption{Same as Fig. \ref{fig:inversion_ff} but for location $B$ (umbra) in Fig. \ref{fig:mapa_GREGOR}, which corresponds to the faint umbra of the sunspot. The physical parameters inferred from the inversion at $\log\tau=-0.5$ are $v=0.43$ km s$^{-1}$, $B=2203$ G, $\gamma=160^{\circ}$, and $\chi=240^{\circ}$, and at $\log\tau=-2.2$ are $v=-0.29$ km s$^{-1}$, $B=2224$ G, $\gamma=158^{\circ}$, and $\chi=240^{\circ}$. }
  \label{fig:inversion_umbra}
\end{figure*}

\section{Results}
\label{sect:results}

The inversion procedures were applied to every spatial position within the FOV of GRIS observations. A median filter was applied to the inversion results to remove the spurious values of the atmospheric parameters retrieved at those individual pixels where the convergence of the inversion is inadequate (at the locations where the differences between the observed and synthetic Stokes spectra resulting from the inversion, quantified by the $\chi^2$, are too high). The value of each parameter at a certain optical depth and spatial coordinates $X$ and $Y$ was substituted by the median in a 3$\times$3-pixel neighborhood.

\subsection{Examination of the atmosphere}
\label{sect:examination}

Figures \ref{fig:mapa_t}\,-\,\ref{fig:mapa_Bincl} show maps of temperature, LOS velocity, and magnetic field strength and orientation for the same region and time illustrated in Fig. \ref{fig:mapa_GREGOR}. The contour lines indicate the masks defined in Fig. \ref{fig:mapa_GREGOR}. Maps at three different atmospheric levels, corresponding to $\log\tau=0.3$, $-0.5$, and $-2.2$ are plotted. As pointed out in Sect. \ref{sect:inversion}, the two higher layers correspond to the peaks in sensitivity of the \mbox{Ca\,\specchar{i}}\ and \mbox{Si\,\specchar{i}}\ lines to the magnetic field, while $\log\tau=0.3$ is the deepest layer where we consider that our inversion results are trustworthy.

The general structure of the sunspot is consistent with a vast number of earlier studies \citep[\rmit{e.g.}][]{Lites+etal1993b,delToroIniesta+etal1994, Stanchfield+etal1997, WestendorpPlaza+etal2001, BelloGonzalez+etal2005, Langhans+etal2005, Balthasar+Collados2005, BellotRubio+etal2007, Beck2008, Balthasar+Gomory2008, Tiwari+etal2015}. The top panel of Fig. \ref{fig:average_atms} shows the variation with optical depth of the temperature averaged over the regions delimited by the masks defined in Fig. \ref{fig:mapa_GREGOR}. At lower atmospheric heights there is a stark contrast between the temperature of dark umbra, faint umbra, and the other regions. Below $\log\tau=-0.6$ the light bridge shows quiet Sun temperatures and for $\log\tau$ between $-0.6$ and $-2$ its temperature is even higher than that of quiet Sun. At the higher atmosphere the light bridge temperature exhibits a steep gradient, reaching an umbral value around $\log\tau=-3$.

\begin{figure}[!ht]
 \centering
 \includegraphics[width=9cm]{mapa_t_mu0o977_deconv.eps}
  \caption{Temperature map inferred from simultaneous inversions of \mbox{Ca\,\specchar{i}}\ 10839 \AA\ and \mbox{Si\,\specchar{i}}\ 10827 \AA\ lines at $\log\tau=-2.2$ (top panel), $\log\tau=-0.5$ (middle panel), and $\log\tau=0.3$ (bottom panel). Contour lines correspond to the same masks as defined in Fig. \ref{fig:mapa_GREGOR}.}
  \label{fig:mapa_t}
\end{figure}

The two deeper velocity maps from Fig. \ref{fig:mapa_vLOS} show clearly the Evershed flow \citep{Evershed1909}. Interestingly, at $\log\tau=0.3$ the light bridge shows an upflow with a velocity of $-1$ km s$^{-1}$ surrounded by two downflows, the strongest with a velocity of 2 km s$^{-1}$. These flows are present only in the side of the light bridge next to the small umbra. The downflows decrease with height and completely vanish by $\log\tau=-2.2$ (top panel). The upflow keeps its value of around $-1$ km s$^{-1}$ for all the optical depths analyzed.

The atmospheres obtained from the inversion are referred to a system of reference with the vertical directed along the LOS. Due to the position of the active region on the solar disk, this reference frame does not coincide with the local reference frame, where vertical magnetic fields are radially oriented. The magnetic field has been transformed to the solar local reference frame. The strength and orientation of the magnetic field are illustrated in Figs. \ref{fig:mapa_Bstrength} and \ref{fig:mapa_Bincl}. At the three plotted optical depths, the photospheric magnetic field ranges from 3000 G strength and a nearly vertical orientation at the center of the umbra to 1000 G and more horizontal inclination at the penumbra. At the deepest layer ($\log\tau=0.3$) the inclination of the penumbral magnetic field is higher, showing values around 90$^{\circ}$ and even reversals.

At the lower atmosphere the light bridge shows a strong reduction of magnetic field strength, with the lowerst trustworthy value as low as 30 G, and becomes more horizontal. At some locations this low magnetic field results in a polarity reversal. The light bridge average field inclination at the deepest layer is 76$^\circ$, but at certain locations its inclination is around 25$^\circ$. Figure \ref{fig:average_atms} shows that for heights below $\log\tau=-0.5$ the magnetic field in the light bridge is more horizontal and has lower strength than the penumbral magnetic field. At higher levels its strength increases to above that of the penumbral average and at the same time it becomes more vertical. The configuration of the magnetic field in the light bridge around $\log\tau=-2.2$ is closer to the faint umbra than the penumbra, according to its inclination of around 150$^\circ$ and its higher strength. The topology of the magnetic field in the light bridge can be pictured as a region with low horizontal magnetic field (including strong reversals in the magnetic field lines) covered by a canopy of stronger and more vertical field, similar to the surrounding umbral field \citep{Jurcak+etal2006, Lagg+etal2014,Schlichenmaier+etal2016}.

\begin{figure}[!ht]
 \centering
 \includegraphics[width=9cm]{mapa_vLOS_mu0o977_deconv.eps}
  \caption{Same as Fig. \ref{fig:mapa_t} but for LOS velocity. Color scale is saturated between -2 and 2 km s$^{-1}$.}
  \label{fig:mapa_vLOS}
\end{figure}

\begin{figure}[!ht]
 \centering
 \includegraphics[width=9cm]{mapa_Bstrength_mu0o977_deconv.eps}
  \caption{Same as Fig. \ref{fig:mapa_t} but for magnetic field strength.}
  \label{fig:mapa_Bstrength}
\end{figure}

\begin{figure}[!ht]
 \centering
 \includegraphics[width=9cm]{mapa_Bincl_localframe_deconv.eps}
  \caption{Same as Fig. \ref{fig:mapa_t}  but for magnetic field inclination in the local solar reference frame. Black arrows indicate the direction of the horizontal magnetic field.}
  \label{fig:mapa_Bincl}
\end{figure}

\begin{figure}[!ht]
 \centering
 \includegraphics[width=9cm]{average_atms_deconv.eps}
  \caption{Stratification of the atmospheric parameters averaged over the region delimited by the masks defined in Figure \ref{fig:mapa_GREGOR}. From top to bottom: temperature, magnetic field strength, and LOS magnetic field inclination. Thick solid line: dark umbra; thin solid line: faint umbra, dotted line: penumbra; dashed line: light bridge; dashed-dotted line: quiet Sun (only in top panel).}
  \label{fig:average_atms}
\end{figure}

\subsection{Geometrical scale}

The optical depth scale ($\log\tau$) retrieved with SIR has been converted to a geometrical scale ($z$) assuming hydrostatic equilibrium. At each location, the hydrostatic equilibrium has been reevaluated taking into account magnetic pressure, but neglecting magnetic tension. Next, the geometrical height has been obtained from the new density and the opacity evaluated at a continuum wavelength. Due to the Wilson depression, the reference height of the geometrical scale for each position is different. We have chosen to define $z=0$ at the height of $\log\tau=0$ in the quiet Sun atmosphere. All the inverted atmospheres have been shifted in the vertical direction in order to look for the configuration that satisfies the pressure balance. In the sunspot this is given by \citep[\rmit{e.g.},][]{Mathew+etal2004}:

\begin{equation}
P_0(z)=P_\mathrm{g}(r,z)+B_\mathrm{z}^2(r,z)/(2\mu_0),
\label{eq:MHS}
\end{equation}

\noindent where $P_0(z)$ is the gas pressure stratification in the quiet Sun, $P_g(r,z)$ is the gas pressure in the spot, $B_z(r,z)$ is the vertical magnetic field, and $\mu_0$ is the magnetic permeability. The curvature force has been neglected, similarly to previous works \citep[\rmit{e.g.}][]{SanchezAlmeida2005, Mathew+etal2004}. For a discussion of the influence of magnetic tension on the estimation of the Wilson depression see \citet{MartinezPillet+Vazquez1993} and \citet{Solanki+etal1993}. We have determined $P_0(z)$ as the average of the gas pressure over all the quiet Sun surrounding the sunspot. The Wilson depression $\Delta z_\mathrm{WD}(x,y)$ is determined as the shift in $z$ which needs to be applied to the total pressure (gas and magnetic pressure) at every position $[x,y]$ in order to match $P_0$ at $\log\tau=0$ (that we have set as $z=0$ in the quiet Sun). This method proved to be problematic when determining $\Delta z_\mathrm{WD}(x,y)$ in the umbra and regions with high magnetic field strength. In those cases, for all the heights where the response functions of the spectral lines are large enough, the total pressure in the magnetized atmosphere was higher than $P_0(z=0)$. This can be partially due to the fact that the gas pressure retrieved from the inversion might be inaccurate in the magnetized regions, since the inversion code does not include the magnetic pressure term in the derivation of the pressure scale. We have determined the change in the Wilson depression of every position with respect to an arbitrarily chosen location with a moderate field strength, instead of the average quiet Sun. In the quiet Sun atmosphere, the range of heights where the inversion provides a reliable result spans around 450 km, while typical Wilson depressions can be higher than 600 km. This means that in some umbral regions the vertical displacement required for matching the photospheric pressures is higher than the available atmosphere. The total pressure stratification of the reference atmosphere is between the low (quiet Sun) and strong (umbra) field cases and the geometrical shift can be directly obtained at all locations. The absolute Wilson depression has been then retrieved by adding the shift between the average quiet Sun and the reference position.

Our estimation of the Wilson depression has some limitations. First, we have neglected the magnetic tension. A rigorous determination would require solving the magnetohydrodynamic equations on a three dimensional grid. The motion equation could be solved even including the velocity and its gradients, although in this case we would miss information about the horizontal components and the temporal derivatives. In addition, the stratification of the parameters retrieved from the inversion imposes some restrictions that will prevent us from obtaining a physical solution due to the uncertainties in the determination of the magnetic field out of the optimal sensitivity region of the spectral lines. Accounting for all this complexity is a huge challenge and is out of the scope of this paper \citep[see][for an example where the Lorentz force is included in the force balance equation]{Puschmann+etal2010}. Finally, we have obtained $\Delta z_\mathrm{WD}(x,y)$ by imposing pressure balance at one specific height. The balance is not satisfied at all $z$ and, thus, choosing a different height as a reference would lead to some differences in the Wilson depression.

\begin{figure}[!ht]
 \centering
 \includegraphics[width=9cm]{mapa_WD_deconv.eps}
  \caption{Wilson depression of the observed sunspot. Contour lines correspond to the masks defined in Figure \ref{fig:mapa_GREGOR}.}
  \label{fig:WD}
\end{figure}

Figure \ref{fig:WD} illustrates the Wilson depression inferred for the observed sunspot. The maximum value of the Wilson depression is almost 600 km. We obtain average values for $\Delta z_\mathrm{WD}(x,y)$ around 500 km for the dark umbra, 330 km for the faint umbra, 110 km for the penumbra, and 8 km for the light bridge. The light-bridge photosphere is basically at the height of the quiet Sun photosphere and at some point its Wilson depression is -100 km, that is, the surface at those locations is above the average surface of the quiet Sun. The contrast in $\Delta z_\mathrm{WD}(x,y)$ of the light bridge with respect to the dark surrounding regions is in the range 200-400 km, in agreement with previous measurements \citep[\rmit{e.g.},][]{Lites+etal2004}.

\subsection{Three-dimensional structure}
\label{sect:3D}
The two-dimensional maps of the solar surface scanned during the observations and the depth-dependent stratification of the inferred physical parameters obtained with SIR allow us to construct a three-dimensional model of the observed active region. Figure \ref{fig:3D} illustrates the thermodynamic and magnetic structure of the sunspot in the local reference frame after transforming the optical depth scale of the stratification into a geometrical scale taking into account the Wilson depression. All the parameters are plotted for $\log\tau$ lower than 0.3, so that we are only including the region where the sensitivity of the spectral lines is high enough.

The top panel of Fig. \ref{fig:3D} shows the region presented in Figs. \ref{fig:mapa_t}\,--\,\ref{fig:mapa_Bincl}, with the horizontal direction expressed in megameters and the position $(x=0,y=0)$ corresponding to the center of the umbra. The continuum intensity is plotted at the surface $\log\tau=0$. Magnetic field lines exhibit a radial geometry. Their color scale illustrates the magnetic field strength at the corresponding location. At the dark umbra magnetic field lines are mostly vertical and their strength is above 2000 G (red). As farther regions from the center of the sunspot are considered, the magnetic field strength is reduced and its inclination is increased until it reaches the penumbra, where comparatively horizontal magnetic field lines dominate. In this panel, the field lines are plotted only where the magnetic field strength is above 500 G.

For a more detailed analysis of the light bridge, the middle panel of Fig. \ref{fig:3D} shows an expanded plot of the domain delimited by the light blue box in the top panel. The point of view of the middle picture is indicated by the ``eye'' in the top panel. In this plot, the $z$-scale has been increased by a factor of 3 in order to better illustrate the Wilson depression. Some selected field lines that cross the light bridge have been plotted in order to illustrated the magnetic field configuration. The center of the umbra is pushed down almost 600 km with respect to the quiet Sun surface. The light bridge shows a remarkable variation of the height at which the continuum intensity is formed, since it comes from a layer between 200 and 400 km higher than the $\log\tau=0$ height at both sides. A movie showing the three-dimensional structure of the light bridge is available in the online material.

Figure \ref{fig:beta} illustrates the plasma-$\beta$ at a surface with constant optical depth $\log\tau=0$ on a logarithmic scale. In the umbra (dark and faint), the isosurface $\log\tau=0$ lies above the $\beta=1$ surface, indicating that the continuum is formed in a low-$\beta$ regime, where magnetic pressure is higher than gas pressure. The photospheric umbra is dominated by magnetic field with plasma-$\beta$ values as low as 0.2. At the penumbra the photosphere change from a magnetic dominated regime at the umbra-penumbra boundary to a plasma dominated regime at the penumbra-quiet Sun boundary. Strong variations in the plasma-$\beta$ associated with penumbral filaments are found at the west side of the penumbra. On the one hand, bright penumbral filaments exhibit plasma-$\beta$ roughly between 10 and 1000. On the other hand, plasma-$\beta$ in dark penumbral regions is around unity. The light bridge shows a striking increase in the plasma-$\beta$. The small umbra at the east side of the light bridge is dominated by magnetic pressure, with a plasma-$\beta$ around 0.2. However, in the light bridge the plasma-$\beta$ is in the range 1-200.

\begin{figure*}[!ht]
 \centering
 \includegraphics[width=14cm]{Figura3D_completa.eps}
  \caption{Three-dimensional structure of the sunspot in the local reference frame. Continuum intensity is plotted at constant $\log\tau=0$ in grey scale. Magnetic field lines are illustrated with a color scale showing the magnetic field strength at the corresponding location from lower than 200 G (purple) to higher than 2000 G (red). Middle panel: detailed view of the light bridge region (delimited by the light blue box in the top panel and from the point of view indicate by the eye in top panel) and some selected field lines obtained from the analysis of the deconvolved maps (see Section \ref{sect:PSF}); bottom panel: detailed view of the light bridge region (same region illustrated in middle panel) and some selected field lines obtained from the analysis of the original non-deconvolved maps (see Sect. \ref{sect:PSF}). In the middle and bottom panels the $z$-axis has been expanded by a factor three.}
  \label{fig:3D}
\end{figure*}

The dynamics of the light bridge are clearly dominated by plasma motions and this fact has a critical relevance for reshaping the magnetic field. The aforementioned velocity flows, consisting of a 1 km s$^{-1}$ upflow surrounded by two downflows with a magnitude of 2 km s$^{-1}$ at $\log\tau=0.3$ and decreasing with height, indicates that the light bridge exhibits vigorous convection. Since in the light bridge the magnetic field is frozen to the plasma motion, magnetic field lines are bent and become more horizontal just on top of the $\log\tau=0$ surface. At some locations they are even completely reversed, exhibiting a change in the polarity of the magnetic field. The bending of the field lines produced by the convective motions is cleary visible at the purple section of the field lines plotted in the middle panel of Fig. \ref{fig:3D}.

The small umbra at the east side of the light bridge imposes a strong almost vertical magnetic field (red vertical field lines in the middle panel of Fig. \ref{fig:3D}). When the field lines crossing the light bridge reach those originating at the small umbra, the magnetic field tension is strong enough to reverse again the direction of the field lines. At those locations, they point in the same direction as they did before crossing the light bridge. Field lines return to a close to vertical configuration, joining at some height the magnetic field lines from the other side of the light bridge (middle panel of Fig. \ref{fig:3D}).

Across the light bridge the magnetic field strength is significantly reduced. The variation of the magnetic field (in comparison with the surrounding dark umbra) decreases with height and goes from around $\Delta B_\mathrm{ch}=2200$ G at $z=0$ to $\Delta B_\mathrm{ch}=1000$ G at $z=1$ Mm. As pointed out before, magnetic field lines form a canopy. Below this canopy the magnetic field strength is even lower.

\begin{figure}[!ht]
 \centering
 \includegraphics[width=9cm]{mapa_beta_deconv.eps}
  \caption{Plasma-$\beta$ at $\log\tau=0$ in logarithmic scale. Contour lines correspond to the masks defined in Figure \ref{fig:mapa_GREGOR}.}
  \label{fig:beta}
\end{figure}

\subsection{Original vs deconvolved maps}
\label{sect:original_deconvolved}

The analysis of the sunspot has been repeated using the original maps instead of those obtained from the deconvolution discussed in Sect. \ref{sect:PSF}. The deconvolution allowed us to take into account the PSF of the telescope (including the effect of seeing) and correct the stray light contamination.

In both cases we obtain a similar global structure. The umbral and penumbral magnetic field show a radial structure. Regarding the light bridge, both cases point to a cusp-like magnetic field configuration, with a lower magnetic field below the canopy and a more vertical field at higher layers. However, there are also significant differences. The canopy obtained from the original maps is formed by mainly horizontal magnetic fields. Some reversals in the field polarization are also measured and small deviations of the field lines from the horizontal are found. However, their bending is barely visible in the bottom panel of Fig. \ref{fig:3D}, which shows results obtained from the analysis of the original data for the same region plotted in the middle panel of that figure. On the contrary, the deconvolved map shows clear signatures of the twisting of the field lines produced by convective motions.

These light bridge convective motions, clearly visible in the velocity map retrieved from the analysis of the deconvolved map, are absent in the flow inferred from the original map. The later only exhibits a 2 km s$^{-1}$ downflow at the side of the light bridge next to the small umbra.

Our estimation of the Wilson depression in the deconvolved map (around 600 km in the umbra) is higher than that obtained by \citet{Mathew+etal2004} using a similar approach (around 400 km) and agrees with that retrieved from geometric techniques using the Wilson effect \citep[600$\pm$200 km][]{Gokhale+Zwaan1972}. \citet{Mathew+etal2004} consider that the difference in their derived Wilson depression is due to neglecting the magnetic tension. However, from the analysis of the original map, the maximum Wilson depression that we obtain in the umbra is slightly higher than 300 km. This result is closer to the value given by \citet{Mathew+etal2004}, and significantly lower that the one inferred with a better resolved map.

The magnitude of the Wilson depression inferred from the original data is strikingly lower than that from the deconvolved map. This effect is specially evident at the light bridge. The height of the $\log\tau =0$ surface around the light bridge in the deconvolved and original maps is illustrated in the middle and bottom panels of Fig. \ref{fig:3D}, respectively. The height difference between the low field strength regions and their surroundings retrieved from the analysis of the original map is below 100 km, while in the deconvolved map this jump is up to 400 km, in agreement with \citet{Lites+etal2004}.

\section{Discussion and conclusions}
\label{sect:conclusions}

We have analyzed the magnetic topology and thermodynamic structure of parts of a sunspot in active region NOAA 12096 a few days before it completely decayed. Our analysis has been focused on the photosphere, with special attention to the magnetic configuration of the deep photosphere that can be explored thanks to the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line. This spectral line is sensitive to deeper layers than other commonly used photospheric lines.

The inversion of the active region reveals many well known and widely explored sunspot properties. Among other features, we have shown the temperature structure and stratification of the sunspot atmosphere, traces of the Evershed flow, changes in the magnetic field from strong and vertical in the umbra to weaker and mostly horizontal in the penumbra, and Wilson depression all over the active region. The most compelling feature for further exploration is the deep photosphere in the light bridge that was formed between the main umbra and a nearby small umbral region. The magnetic field at this location is not only much lower than in the surrounding umbral regions, but also lower than the penumbral magnetic field. At the same time, its inclination with respect to the local vertical is also lower, showing horizontal field lines and even reversals in their trajectory. The vertical stratification of the light bridge atmosphere is clearly different from other penumbral regions.

The magnetic field structure of the light bridge reveals several similarities with the configuration that has been found for previously analyzed light bridges: it exhibits lower and more horizontal magnetic field relative to the umbra \citep{Beckers+Schroter1969, Lites+etal1991,Leka1997}, its brightness is similar to the penumbra and it separates two regions with the same polarity \citep{Sobotka+etal1993, Rimmele2008}, the higher layers are comparable to the surrounding umbral atmosphere \citep{Ruedi+etal1995}, and the field lines form a cusp-like structure with a reduced field region in the inner part \citep{Leka1997, Jurcak+etal2006, Lagg+etal2014}. In addition, the velocity profile shows central hot upflows surrounded by cooler downflows. This flow pattern has been detected in other light bridges and it is interpreted as a evidence for vigorous convection in the light bridge \citep{RouppevanderVoort+etal2010, Lagg+etal2014}.

The flow pattern measured for the light bridge exhibits some differences with respect to those observed in previous analyses. In this light bridge we do not detect a complete convective cell, where the upflow is completely surrounded by downflows. Instead, we have only detected downflows at the side of the light bridge closer to the small umbra. The width of this cell (1.9\hbox{$^{\prime\prime}$}) is comparable to the typical width of quiet-Sun granules and those observed in light bridges \citep[$1-2$\hbox{$^{\prime\prime}$}][]{Lagg+etal2014}. Only one of these convective cells is found in the analysed light bridge, whose convective motions resemble those from quiet-Sun granules, except for the asymmetry in its downflows. The light bridge is relatively small, and it is possible that missing convective downflows are spatially unresolved near the umbral edges of both sides of the light bridge. Pressure and horizontal motions towards the edges of the light bridge could squeeze these downflows to very small spatial scales, out of the reach of the spatial resolution achieved even with the deconvolution described in Sect. \ref{sect:PSF}, since the small-scale stray light could not be properly characterized. We also find some signatures of convection in the flow pattern at the centre side of the penumbra (see the range x=[25\hbox{$^{\prime\prime}$}, 28\hbox{$^{\prime\prime}$}] and y=[6\hbox{$^{\prime\prime}$}, 8\hbox{$^{\prime\prime}$}] from bottom panel of Fig. \ref{fig:mapa_vLOS}). The presence of convective motions in the penumbra has been pointed out by previous observational works \citep{Ichimoto+etal2007,Zakharov+etal2008, Joshi+etal2011, Scharmer+etal2011, Tiwari+etal2013}.

As discussed in Sect. \ref{sect:evolution}, the light bridge is created by the motion of a small umbral region towards the main umbra (see movie). It is composed of the penumbral and quiet Sun atmosphere that remained confined between two highly magnetized regions at the time the analysed data were acquired. As the two magnetized regions approach each other, the field lines that spread from the central umbra are blocked by those coming from the dark pore-like feature. The field lines above the light bridge are forced to become more vertical than in the rest of the penumbra (see bottom panel of Fig. \ref{fig:average_atms} around $\log\tau=-2$). This process forms a magnetic canopy. An atmosphere with very low magnetic field and quiet Sun temperature (see top and middle panel of Fig. \ref{fig:average_atms}) remains covered by a cusp-like field configuration. Convection keeps working, but the flows are confined by the low-$\beta$ atmosphere of the surrounding umbrae. Below the canopy, gas pressure is much higher than magnetic pressure (plasma-$\beta$ in the range 10-200). The downflowing material due to convection can drag down towards the interior the magnetic field below the canopy, bending the field lines and leading to reversals in the field orientation. Closer to the small umbra the magnetic tension can reverse again the field lines, which recover an almost vertical configuration and join the vertical field lines from the other side of the umbra.The magnetic canopy confines the plasma to the lower atmosphere. An example of this phenomena was recently found by \citet{Louis+etal2015}, who reported the emergence of a small loop in the lower atmosphere of a sunspot light bridge. The loop does not reach the chromosphere since the magnetic field configuration impedes it from continuing rising.

Field lines reversals in light bridges were recently detected by \citet{Lagg+etal2014}. They proposed two possible scenarios: the field lines reverse their direction again due to magnetic tension, or the field is dragged towards the interior and the field lines are then downward directed. Our results have confirmed the presence of bending in the field lines and have shown evidence that their first scenario is the most plausible. The detection of the two successive reversals in the field lines is only possible thanks to the high sensitivity of the \mbox{Ca\,\specchar{i}}\ 10839 \AA\ line to the deep layers and the high spatial resolution of GREGOR telescope. Many works have reported chromospheric activity phenomena above light bridges \citep[\rmit{e.g.},][]{Roy1973,Asai+etal2001,Berger+Berdyugina2003,Shimizu+etal2009,Toriumi+etal2015,Robustini+etal2016}. Our observations in \mbox{He\,\specchar{i}}\ 10830 \AA\ do not show any trace of these dynamics events. However, the magnetic configuration found in our work at the deep photosphere can trigger those phenomenon through reconnection of the reversed field lines.

The inversions carried out in this paper have been independently performed using the original map and the spatially deconvolved map, which takes into account the telescope and seeing PSF and the stray light contamination. Both results show a similar general picture. However, the inversion of the original map also present significant differences with the analysis of the deconvolved map. First, it does not reveal a clear pattern of the overturning convective motions of the light bridge. Instead, only a downflow is obtained. Second, the complex bending of the field lines in the light bridge is not undoubtedly detected. Opposite polarity fields are also found in the original non-deconvolved maps, but the curvature of the field lines is much lower. Finally, the magnitude of the Wilson depression is greatly underestimated. Our results indicate the remarkable relevance of correcting for telescope resolution and stray light in order to infer the magnetic and thermodynamic structure of the Sun from spectropolarimetric observations.

The decay of a sunspot is a long process during which the structure of the atmosphere shows a striking and complex evolution. Our analysis revealed the magnetic field configuration of the lower photosphere at a specific time close to the final stages of a sunspot. A comprehensive study of the magnetic configuration during the decay will require tracking an active region over several days. This study would also benefit from the inclusion of many active regions, sampling each stage of the evolution at different positions on the solar disk in order to analyze the magnetic and thermodynamic configuration under different viewing geometries.

\begin{acknowledgements}
The authors thank Basilio Ruiz Cobo and Carlos Quintero Noda for advice on inverting the data and providing very useful suggestions. The 1.5-meter GREGOR solar telescope was built by a German consortium under the
leadership of the Kiepenheuer-Institut f\"ur Sonnenphysik in Freiburg with the
Leibniz-Institut f\"ur Astrophysik Potsdam, the Institut f\"ur Astrophysik
G\"ottingen, and the Max-Planck-Institut f\"ur Sonnensystemforschung in G\"ottingen as
partners, and with contributions by the Instituto de Astrof\'isica de Canarias and
the Astronomical Institute of the Academy of Sciences of the Czech Republic. SDO HMI data are provided by the Joint Science Operations Center - Science Data Processing. The support of the European Commission's FP7 Capacities Programme under Grant Agreement number 312495 ``SOLARNET'' is acknowledged. This research has been funded by the Spanish MINECO through grant AYA2014-55078-P.
\end{acknowledgements}

\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


Mighty Quinn Productions was developed out of my respect for music and the people who make it. Our goal is to reissue recordings by quality artists that have not yet been released on CD, or have sadly fallen out of print. We want to make sure that worthy albums in all genres of music aren't lost or forgotten. We also plan to produce compelling new artists who we believe should be heard. Mighty Quinn is committed to providing the best possible sound for the sake of both the listener and the artist, and we will include intelligent and insightful liner notes to complete a package of overall excellence.
Get Happy - Tiny Grimes exchanges with violin. Tommy Lucas exchange with piano.
Mimi - Tiny Grimes 1st solo. Tommy Lucas 2nd solo with piano exchange.
Hard Day's Night - Intro solo by Tommy Lucas. 8 bars solo by Tiny Grimms.
Stardust - Tommy Lucas. Sequel into Tiny Grimes solo before violin re-enters.
She's Funny That Way - Tommy Lucas. 1st solo then Tiny Grimes before bass solo.
Recorded at Western Recorders Inc. in Hollywood. Cal.
"One of the most distinctive clarinetists of all time, Edmond Hall had an intense sound that would have no difficulty being heard above a brass section. After gaining experience playing in New Orleans in the 1920s (including with the unrecorded cornetist Buddy Petit) and with swing bands in the '30s, most notably that of Claude Hopkins, Hall spent the rest of his career with small groups, including the Louis Armstrong All-Stars for a few years in the 1950s.
Petite Fleur was one of Edmond Hall's very few full-length albums as a leader and was formerly among his rarest. Recorded Dec. 1958, it features Hall on four numbers with a quartet and on four other performances (including a six-song Duke Ellington medley) with a sextet that includes trumpeter Emmett Berry and trombonist Vic Dickenson. It is a pleasure to hear Hall in the spotlight and he really excels, particularly on Sidney Bechet's "Petite Fleur," "Clarinet Marmalade" and a few of his obscure originals. A special treat is the unusual "Don't Give Me Sympathy" which has a good-humored Hall vocal.
The Mighty Quinn label during the past year has been making available a series of long-out-of-print jazz sets from the 1950s and '60s. Its catalog (www.mightyquinn.net) is well worth exploring."


Best Dog Walkers in Linda Vista of San Diego, CA | Wag!
Linda Vista is a neighborhood on the north side of San Diego, California. It is a 15-minute commute south to the city's central business district. There are a variety of local shops, restaurants, and services located along Linda Vista Road that are within walking distance for many residents, however, this area is separate from many of the residential spaces and foot travel to commercial businesses is not always feasible. There is a recreation center and schools in the community that most people and pets can reach on foot.
When walking with your dog in Linda Vista, you will enjoy warm, sunny weather most of the year. Winters are colder, but still mild. Summer days can be very hot, especially in the middle of the day. Some overcast, rainy, and foggy weather is common in spring, but is usually short-lived, and does not prevent outings with your dog.
Linda Vista is bordered by the Cabello Freeway on the east, Friars Road on the south, and the Telcoate Canyon on the west and north sides. The neighborhood is located on a high mesa that provides views of the surrounding communities, wilderness areas, and even views of the Pacific Ocean. The Telcoate Canyon has rough terrain, native flora and fauna, canyons, and hills that extend their "fingers" into the neighborhood's west side.
Most of the Linda Vista neighborhood is residential and comprised of single-family detached homes that are moderate in size and attractively maintained. The terrain, even in the residential areas, can be hilly and you and your dog will need to be prepared to trek up and down some hills to get around.
There are sidewalks along streets, so you and your pet don't have to share the road with local traffic. Golf courses on the northwest and southwest borders of Linda Vista provide manicured green spaces that contrast with the natural terrain nearby.
The Kearny Mesa Dog Park is located on the north side of Linda Vista. This enclosed dog park is an acre in size and has a drinking water supply. Your dog should be supervised in this off-leash park.
The Mission Heights Neighborhood Park is centrally located and has some recreational fields and facilities with a walking path around it. Dogs must remain leashed in this park and you should be prepared to clean up after your pet. The Tecolote Canyon Natural Park on the west side has 6.5 miles of trails that are popular with mountain bikers, joggers, and dog walkers. Your dog should remain leashed and you should watch for other fast-moving trail users. Wildlife in the area can also pose a hazard to your dog, so watch for local critters to avoid unpleasant encounters.
The Linda Vista Community Park has a recreation center and some open green space with walking trails where you can stroll with your leashed pet.


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Caldwell, Bruce, Louis Scatt, and Henry M. Tipton. Economic Progress: Fact or Fantasy? Columbia: U of Missouri P, 1991. Print.
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McCarthy, Ann. "Talking to the Walls." Great Science Fiction Tales. Ed. Harry Green, Moe Black, and Maggy Brown. New York: Doubleday, 1985. 177-188. Print.
Article from Online Database – IF USING EBSCO/SIRS THIS WILL BE CREATED FOR YOU!!
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Kaestle, Christine E., and Martha W. Waller. "Bacterial Stds And Perceived Risk Among Sexual Minority Young Adults." Perspectives On Sexual & Reproductive Health 43.3 (2011): 158-163. Academic Search Elite. Web. 7 Mar. 2013.
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text:
Slovakia´s unemployment rate at its new minimum in March, the lowest number since 1993
Slovakia´s registered unemployment rate amounted to 5.03% in March, from 5.16% in February, down by 0.13 percentage points (pp) month-to-month and by 0.52pp year-on-year
By bne IntelliNews April 24, 2019
Slovakia´s registered unemployment rate amounted to 5.03% in March, from 5.16% in February, down by 0.13 percentage points (pp) month-to-month and by 0.52pp year-on-year, according to data published by the Labour, Social Affairs and the Family Centre on April 23.
The number of jobseekers immediately able to start work was recorded at 137,962 persons. The rate of unemployment calculated from the total number of jobseekers stood at 6.19%, down by 0.16pp m/m and by 0.58pp y/y.
"The number decreased by 3,470 m/m while in yearly terms it dropped by 15,892 persons, which is by 10.33% less," stated the Centre General Manager Marian Valentovic, adding that the total number of jobseekers in March stood at 169,779 persons, dropping by 4,294 persons m/m and 17,980 persons y/y (by 9.58% less), as online eTrend.sk quoted.
The monthly rate decrease of registered unemployment was recorded in all regions, with Presov region posting the most significant fall. The unemployment rate dropped below 4% in 36 districts, according to the Labour Minister Jan Richter (Smer-SD). Most jobs were offered in Bratislava region, the least in Banska Bystrica. By the end of March there were 88,093 available jobs, up by 1,961 open positions m/m.
According to the minister, the development of March unemployment rate returned to "positive numbers". He stressed he expects the rate to decrease below 5% in April.
Despite people going hungry amid economic crisis ruling autocrats continue to pile money into vanity projects, while failing to pay contractors. Eight-lane 'Turkmen Autobahn' latest investment to raise eyebrows.
States across Central and Southeast Europe are experiencing a long-term population decline due to a combination of low birth rates and mass emigration.
Prices of food (down 1.1% m/m), clothes and footwear (down 3.0%) and utilities (down 1.4%) dragged the headline figure down in June.
Russia's current account posted a $45.6bn surplus in the first half of this year
Softer crude oil prices offset by weak domestic demand and lower imports all contributed to the surplus
Czech retail sales fell 1% month-on-month at constant prices in May after very strong growth in previous months, and marked the slowest growth in 2 years.